CCD photometry of Seyfert galaxy NGC 1068

Surface photometry of galaxies

“…They showed that BCMs are on the average 1.2 mag brighter than predicted from their velocity dispersions and the L oc a 4 relation (e.g., Kormendy and Illingworth 1983) for ellipticals. These new results may be in contradiction to the current theories of BCM formation through simple homologous mergers (e.g., Ostriker and Hausman 1977;Hausman and Ostriker 1978;Malumuth and Richstone 1984) direct evidence for mergers (Hoessel 1980;Schneider et al 1983;Hoessel, Borne, and Schneider 1985). However, recent measurements of redshifts for a considerable number of multiple-nuclei galaxies (Tonry 1985;Smith et al 1985) have shown that the distribution of the velocity differences between multiple nuclei and the central galaxy has an rms width of ~ 800 km s~\ This large velocity suggests that only a small fraction of the nuclei is moving on bound orbits slowly enough to be captured (Tonry 1984(Tonry , 1985.…”

“…Because of this limitation, recent surface photometry of galaxies appears to be divided into the following four categories: 1. CCD surface photometry using a large telescope or at the slow focal plane of a small-sized telescope of either apparently small galaxies, including QSOs, or bright central regions of relatively nearby galaxies (e.g., Hoessel 1980;Young et al 1980;Hickson et al 1982;Carter et al 1983;Schneider, Gunn, and Hoessel 1983;Gehren et al 1984;Price 1985;Kormendy 1985a,b ;Lauer 1985a;Fort étal. 1986;Jedrzejewski 1987;Daly, Phillips, and Disney 1987).…”

“…Color variation across the face of a galaxy can also be made visible by making the same sort of maps of the color-ratio image, C l2 (x,y) = Sfx,y) ~ S 2 (x,y) ^ = const. -2.5 log l\(x,y)H¿x,y) , where l(x,y) is the relative intensity distribution and the subscripts 1 and 2 discriminate the color bands (Schweizer 1976;Talbot, Jensen, and Dufour 1979;Schild et al 1985;Ichikawa et al 1987a). A pseudocolor map is most convenient to display the color-ratio image, where the actual color variation in the galaxy is imitated.…”

“…Multicolor surface photometry has also been used to estimate stellar populations in different parts of a galaxy (e.g., Jensen, Talbot, and Dufour 1981;Schild et al 1985;Ichikawa et al 1987a). Barred galaxies and ringed galaxies have also been favorite targets, the aim of the studies being the comparison with stellar dynamical models (e.g., Benedict 1982;Blackman 1983;Elmegreen and Elmegreen 1985;Pence and de Vaucouleurs 1985;Duval and Monnet 1985;Buta 1986Buta , 1987a.…”

Host Galaxy Bulge Predictors of Supermassive Black Hole Mass

“…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)…”