CCD surface photometry of galaxies with dynamical data. I - NGC 3379, M87, and NGC 1052

Davis, L. E.; Cawson, M. G. M.; Davies, R. L.; Illingworth, G. D.

doi:10.1086/113723

Cited by 46 publications

(29 citation statements)

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“…Many authors did not find significant variations in the geometry of galaxies obtained in different optical bands (Davis et al 1985;Jedrzejewski 1987;Capaccioli et al 1988;Fasano & Bonoli 1989;Caon et al 1990;Peletier et al 1990;Rampazzo & Sulentic 1992;Reduzzi & Rampazzo 1996). For the nearinfrared band, Elmegreen et al (1996) did not find significant differences in spiral profiles obtained in the JHK bands.…”

Section: An Overviewmentioning

confidence: 96%

Photometric study of a sample of southern binary galaxies

Silva

Souza²

2006

A&A

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Aims. This work exhibits the basic optical photometric data for a sample of 50 probable southern binary galaxies. Our sample covers a broad range of pair separations, stages of interaction, and morphologies. From the initial list of selected pairs, using spectroscopic data from the literature and our own data, we conclude that 84% of these systems are true binary galaxies. Methods. We present residual and asymmetric maps, R major semi-axis profiles of surface brightness, ellipticity, position-angle, harmonic Fourier coefficients of third and fourth order (b 3 and b 4 ) for 50 probable pairs, and B − R color maps for 47 of these pairs. For most galaxies, we present the profiles in two different ways, aiming to verify the influence of random errors on them. Results. We note that random errors in position-angle profiles are at least 2• , but a more significant result must take into account a variation larger than 11• for this distribution. Barred galaxies usually show a typical behavior in ellipticity and position-angle profiles: these profiles display variations when changing from a bar to a disk region. In some cases, the variations also occur along the bar. Some galaxies show distribution profiles that are common for their morphological type, and the interaction signature is only evidenced by their residual maps. Bars are usually redder and rings are bluer, when compared with the galaxy outskirts. Conclusions. Our data indicates that there is a connection between interaction strength and morphological distortions in binary galaxies. If we consider the projected separation of a pair as an indication of interaction strength, distortions such as displaced centers, anomalous shapes of spiral arms, and twistings of external regions are easily detected in some close pairs, although not all components of close pairs show this behavior. Our data suggests that besides interaction, other parameters, like orbital geometry and internal properties of galaxies, can stimulate binary galaxies' peculiarities.

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Section: An Overviewmentioning

confidence: 96%

Photometric study of a sample of southern binary galaxies

Silva

Souza²

2006

A&A

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“…References.-(1) Lauer et al 1998; (2) Peletier 1993; (3) Hoessel & Melnick 1980; ''positions with respect to the center have been multiplied by a factor of 1.035'' as given by Walterbos & Kennicutt 1987;(4) Baggett et al 1998;(5) full profile obtained directly from K. Gebhardt; (6) Gebhardt et al 2003; (7) Lauer et al 1995;(8) Schild et al 1985;(9) Peng et al 2002;(10) de Vaucouleurs et al 1991;(10b) typical value in de Vaucouleurs et al (1991) for other sample galaxies; (11) taken from Gebhardt et al 2000a;(14) Lauer 1985;(15) Peletier et al 1990;(16) Burstein 1979;(17) Davis et al 1985;(18) Kormendy 1977;(19) Michard 1985;(20) Lauer et al 2005;(21) full profile obtained directly from C. Siopis; (22) Siopis et al 2007;(23) Ferrarese et al 1994, with 0.5 mag added to match other data; (24) Ferrarese et al 1996;(25) Scorza & van den Bosch 1998;(25b) Scorza & van den Bosch 1998, Fig. 1;(26) Cretton & van den Bosch 1999;(27) Caon et al 1990;(28) Sarzi et al 2001;(29) Lauer et al 1992a;(30)…”

Section: Surface Brightness Profilementioning

confidence: 99%

Host Galaxy Bulge Predictors of Supermassive Black Hole Mass

Aller

Richstone

2007

ApJ

118

153

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A variety of host galaxy ( bulge) parameters are examined in order to determine their predictive power in ascertaining the masses of the supermassive black holes (SMBHs) at the centers of the galaxies. Based on a sample of 23 nearby galaxies, comprised of both elliptical galaxies and spiral /lenticular bulges, we identify a strong correlation between the bulge gravitational binding energy (E g ), as traced by the stellar light profile, and the SMBH mass (M ), such that M / E 0:6 g . The scatter about the relationship indicates that this is as strong a predictor of M as the velocity dispersion (), for the elliptical galaxy subsample. Improved mass-to-light ratios, obtained with IFU spectroscopy and I-band photometry by the SAURON group, were used for those sample galaxies where available, resulting in an energy predictor with the same slope, but with reduced scatter. Alternative M predictors such as the gravitational potential and the bulge mass are also explored, but these are found to be inferior when compared with both the bulge gravitational binding energy and bulge velocity dispersion predictors, for the full galaxy sample.

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“…The data must also be corrected for seeing effects, galactic extinction, K correction and cosmological dimming. The data from Prugniel & Simien (1996) and Alonso et al (2003) consider all the corrections mentioned above, even though the correction for extinction and the K correction were done using Burstein & Heiles (1984) data and those from Davis et al (1985) respectively. The cosmological corrections were done using (1 + z) 4 .…”

Section: The Sample Of Etg In Coma Clustermentioning

confidence: 99%

Structural properties of isolated early-type galaxies. The dependence of scaling relations on environment

Nigoche-Netro

Moles

Ruelas-Mayorga

et al. 2007

A&A

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Aims. In order to investigate whether gravitational interactions between galaxies are able to modify their structural properties, we determine the Kormendy relation (KR) for a sample of isolated early-type galaxies (ETG) for which we have measured several photometric parameters. This relation is compared with that obtained for a sample of ETG of the Coma Cluster, and with that obtained for a sample of perturbed S0 galaxies contained within high-density environments. Methods. Using very strict physical isolation criteria we selected a sample of 82 E and S0 galaxies from the CfA catalogue, in the redshift range 5000 km s −1 ≤ cz < 10 000 km s −1 . We obtained the photometric parameters, (r e , S B e ) and total magnitude for 21 galaxies in the B filter and for 23 in the Gunn r filter.Results. The main result we obtained is that the KR is the same for isolated galaxies and for galaxies in high-density environments or in interaction. In addition we found evidence that the intrinsic dispersion of the KR depends on the magnitude range within which the galaxies are contained (larger dispersion for larger magnitude range), and not on the degree of gravitational interaction to which these galaxies are subjected.

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CCD surface photometry of galaxies with dynamical data. I - NGC 3379, M87, and NGC 1052

Cited by 46 publications

References 0 publications

Photometric study of a sample of southern binary galaxies

Photometric study of a sample of southern binary galaxies

Host Galaxy Bulge Predictors of Supermassive Black Hole Mass

Structural properties of isolated early-type galaxies. The dependence of scaling relations on environment

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