Hyperleda

Paturel, G.; Petit, C.; Prugniel, Ph.; Theureau, G.; Rousseau, Judith; Brouty, M.; Dubois, P.; Cambrésy, L.

doi:10.1051/0004-6361:20031411

Cited by 836 publications

(860 citation statements)

References 75 publications

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“…Sources: (t) Tonry et al (2001) after reducing their distance moduli by 0.06 mag (Blakeslee et al 2002); (n) from NED (3K CMB). Col. (5) Central velocity dispersion from HyperLeda b (Paturel et al 2003). Col. (6) Filters.…”

Section: Galaxy Imagingmentioning

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

147

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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: Galaxy Imagingmentioning

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

147

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“…We additionally apply a morphological cut based on the Hyperleda database (Paturel et al 2003) to remove large spiral and interacting galaxies. The large-scale environment, group numbers, and halo masses are taken from the 2MASS-based high-density contrast (HDC) group catalog of Crook et al (2007).…”

Section: The Massive Surveymentioning

confidence: 99%

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

112

156

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Studies of the physical properties of local elliptical galaxies are shedding new light on galaxy formation. Here we present the hot-gas properties of 33 early-type systems within the MASSIVE galaxy survey that have archival Chandra X-ray observations, and we use these data to derive X-ray luminosities (L X,gas ) and plasma temperatures (T gas ) for the diffuse gas components. We combine this with the ATLAS 3D survey to investigate the X-ray-optical properties of a statistically significant sample of early-type galaxies across a wide range of environments. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, we deduce that all early types (independent of galaxy mass, environment, and rotational support) follow a universal scaling law such that µL T X,gas gas 4.5 . We further demonstrate that the scatter in L X,gas around both K-band luminosity (L K ) and the galaxy stellar velocity dispersion (s e ) is primarily driven by T gas , with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the gas origin directly to either stellar mass or galaxy potential. Indeed, our data require a steeper relation between L L , K X,gas , and s e than predicted by standard mass-loss models. Finally, we find that T gas is set by the galaxy potential inside the optical effective radius. We conclude that within the innermost 10-30 kpc region, early types maintain pressure-supported hot gas, with a minimum T gas set by the virial temperature, but the majority show evidence for additional heating.

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“…We fitted with Gaussian profiles the Ca II triplet λ 8500.36, 8544.44, 8664.52 Å absorption lines extracted with a 1 ′′ aperture, corresponding to 397, 192, and 92 pc for 2MASX J18305065+0928414, ESO 234-G050, and NGC 6221, respectively. The HyperLeda database (Paturel et al 2003) presents measurements which have been homogenized to a common aperture r HL = 0.595 kpc. In order to convert our σ ⋆ measurements to the common radius r HL we corrected for the aperture effects using the relation σ ⋆ (r) ∝ r −0.066 of Cappellari et al (2006).…”

Section: Sample Selectionmentioning

confidence: 99%

Detection of faint broad emission lines in type 2 AGNs – III. On the MBH-σ⋆ relation of type 2 AGNs

Ricci

Franca

Marconi

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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Type 2 active galactic nuclei (AGN) represent the majority of the AGN population. However, due to the difficulties in measuring their black hole (BH) masses, it is still unknown whether they follow the same BH mass-host galaxy scaling relations valid for quiescent galaxies and type 1 AGN. Here we present the locus of type 2 AGN having virial BH mass estimates in the M BH − σ ⋆ plane. Our analysis shows that the BH masses of type 2 AGN are ∼ 0.9 dex smaller than type 1 AGN at σ ⋆ ∼ 185 km s −1 , regardless of the (early/late) AGN host galaxy morphology. Equivalently, type 2 AGN host galaxies have stellar velocity dispersions ∼ 0.2 dex higher than type 1 AGN hosts at M BH ∼ 10 7 M ⊙ .

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Hyperleda

Cited by 836 publications

References 75 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

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Detection of faint broad emission lines in type 2 AGNs – III. On the MBH-σ⋆ relation of type 2 AGNs

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