S0 galaxy NGC Marcella Carollo, HST.

Transcription

1 S0 galaxy NGC Marcella Carollo, HST.

2 Dust lane in NGC Marina Rejkuba, ESO.

3 Peculiar E galaxy NGC Paul Goudfrooij, HST.

4 Dust-lane E galaxy NGC Carnegie Atlas of Galaxies.

5

6 1994ApJ...43 HI ring around IC This ring is circular and inclined at 37. Franx, van Gorkom, & de Zeeuw (1994). E galaxy IC Carnegie Atlas of Galaxies.

7 1997ASPC M HI disk around NGC Morganti et al. (1997).

8 HI around E and S0 galaxies. Osterloo et al (2007).

9 E galaxy NGC 1132 in optical light and X-rays. Mike West, NASA.

10 23 Jul :25 AR AR194-AA41-06.tex AR194-AA41-06.sgm LaTeX2e(2002/01/18) P1: IKH HOT GAS IN AND AROUND ELLIPTICAL GALAXIES 203 Annu. Rev. Astro. Astrophys : Downloaded from arjournals.annualreviews.org by University of Hawaii at Manoa Library on 01/29/09. For personal use only. Figure 4 Contours show a combined ROSAT HRI and PSPC X-ray image of NGC 4472 X-rays superimposed (contours) onemission an optical from image NGC from 4472 the (after Digital Irwin Sky & Sarazin Survey 1996). (Irwin Mathews & Sarazin & Brighenti 1996). (2003) is similar to the mean profile of about 10 other bright E galaxies out to at least 18 R e. In nonspherical E galaxies, the existence of massive dark halos can be inferred directly from the X-ray image independent of the hot gas temperature

11 HOT GAS IN AND AROUND ELLIPTICAL GALAXIES : Downloaded from arjournals.annualreviews.org i at Manoa Library on 01/29/09. For personal use only. X-ray vs optical luminosity for E galaxies. Mathews & Brighenti (2003). Figure 1 A plot of the bolometric X-ray luminosity and B-band optical luminosity for elliptical galaxies (RC3 type T 4) from the compilation of O Sullivan et al. (2001). X-ray detections are shown with filled circles and upper limits with open triangles. The dashed line is an approximate locus of the total luminosity L x, L B of stellar and other discrete sources also from O Sullivan et al. (2001).

12 X-ray spectrum of NGC BM98 fig 8.8.

13 Specific frequency of globular clusters vs magnitude (left) and Hubble type (right). BM98 fig 4.63

14 Metallicity of GCs in NGC 5128 (shaded) and MW. Held et al. (1997).

15 Young (blue) and old (red) globular clusters in E galaxy NGC Puzia et al. (2002).

16 Left: spectra of K0 star (S) and galaxy NGC 2549 (G). Right: galaxy (dotted) and model (solid). BM98 figs 11.1, 11.4.

17 Major-axis kinematics of giant E galaxies (after Carollo et al. 1995). BM98 fig

18 Left: major-axis and minor-axis kinematics of NGC Right: kinematic misalignments for E galaxies. BM98 figs. 11.9,

19 N PNs in NGC Peng, Ford, & Freeman (2004).

20 Radial velocities of PN in NGC Peng, Ford, & Freeman (2004).

21 Smoothed, symmetrized PN velocities. Peng, Ford, & Freeman (2004).

22 Kinematically decoupled cores in two E1 galaxies. Schweizer (1998).

23 Color maps of E galaxies with decoupled cores; red is dark, each is 6 square. Carollo et al. (1997).

24 Major-axis coord. Velocity profiles for S0/E7 galaxy NGC de Zeeuw (1994).

25 Top: Low-order basis functions. Bottom: effects on Gaussian (dotted) profiles. van der Marel & Franx (1993).

26 Major-axis kinematics of giant E galaxies (after Carollo et al. 1995). BM98 fig

27 Annu. Rev. Astro. Astrophys : Downloaded from arjournals.annualreview by University of Hawaii at Manoa Library on 01/30/09. For personal use only. quivalent relation is obtained for luminosity. The old Faber- Jackson and radius-surface brightness relations are projections of the fundamental plane. The luminosity-color and mass-metallicity relations are also contained in the fundamental plane. Its tilt with respect to the R -e I ~ " " ".,:, I I I I I I " </~>o log t~ ~: log tr - R ~t log o" </~>,, Figure 2 Projections of the fundamental parameter plane of elliptical galaxies. Top panels: the one-parameter scaling relations discussed in Section 8.2, i.e. (left) the relation between radius and mean surface brightness, and (right) that between luminosity and velocity dispersion (the Faber-Jackson relation). Bottom left: the surface brightness-velocity dispersion correlation is the fundamental plane seen almost face-on. This is an observer s version of the cooling diagram from theories of galaxy formation. Bottom riyht: this relation between the radius and a combination of surfa Projections of the fundamental plane. Kormendy & Djorgovski (1989).

28 1995ApJ F Central velocity dispersion vs Mg b index for Es (open) and BCGs (filled). Fisher et al. (1995).

29 1997AJ F Break radius vs magnitude. Faber et al. (1997).

30 L120 KORMENDY & BENDER Vol. 464 FIG. 1. Proposed morphological classification scheme for elliptical galaxies. Ellipticals are illustrated edge-on and at ellipticity The connection between boxy and disky ellipticals may not be continuous (see 4). This figure is based on the tuning-fork diagram of Hubble (1936). We make three additional modifications: we illustrate the two-component nature of S0 galaxies and label them as barred or unbarred, we call unbarred spirals ordinary Kormendy rather than & Bender normal (1996). (de Vaucouleurs 1959), and we add Magellanic irregulars. 2. CLASSIFICATION SCHEME FOR ELLIPTICAL GALAXIES Figure 1 illustrates the proposed classification. Smoothly connecting onto S0 s are disky ellipticals, i.e., those with isophotes that are more elongated along the major axis than best-fitting ellipses. Next come boxy ellipticals, i.e., those with isophotes that are more rectangular than ellipses. We illustrate the classification with Hubble s (1936) tuning-fork diagram; clearly, it can be incorporated into de Vaucouleurs (1959) more detailed classification. Ellipticals with exactly elliptical isophotes are omitted; we consider them to be intermediate between disky and boxy 3. EVIDENCE THAT ISOPHOTE SHAPES MEASURE ANISOTROPY Our discussion of isophote shapes follows Bender et al. (1989, hereafter B 89) and Kormendy & Djorgovski (1989). Evidence that a 4 /a measures anisotropy is summarized in Figure 2. The upper panel plots (V/ )*, the ratio of the rotation parameter V/ to the value for an isotropic oblate spheroid flattened by rotation (Davies et al. 1983; V is the maximum rotation velocity, and is the mean velocity dispersion inside one-half of the effective radius). The correlation of (V/ )* with a 4 /a shows that rotation is dynamically less important in boxy than in disky ellipticals (Bender 1987, 1988; Nieto, Capaccioli, & Held 1988; Wagner, Bender, & Möllen-