Galaxies: Classification. Galaxy Classification. galaxies; late types : spiral galaxies, Not an evolutionary sequence!

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1 17 1 Galaxies: lassification Galaxy lassification s: Hubble and others: classification of galaxies orphology: ppearance on photographs, photographic emulsion is blue sensitive Warning: scheme is in parts not so well defined, incomplete, and not unique ote: photometric (colors) and spectroscopic information are not part of the Hubble scheme. SDSS Galaxy classification via the Hubble tuning fork diagram : early types : elliptical galaxies; late types : spiral galaxies, ot an evolutionary sequence! 87 (=irgo, note jet; 0), OO/U/S O X D O X D D D D S D S

2 49 (4), OO/U/S 59 (5; color image), OO/U/S 86 (lenticular, S0), OO/U/S D O D 17 8 lliptical Galaxies X D S lliptical galaxies: lassification as x where x = 10(a b)/a (integer part; between 0 and 7) llipticals are low on dust and gas, reddish color (=old stars!), typically low luminosity and low mass (10 6 ) onsters: lso elliptical, from mergers in galaxy clusters (e.g., 87 in irgo), up to 10 12, designated cd. 60 (G 4649), 1, U. of labama lliptical Galaxies 5

3 104 (Sa; Sombrero galaxy ), HST/S dge on Spiral G 4013 (Sa; S/HST) D O D 17 9 lliptical Galaxies X D S aroll & Ostlie ig. 25.2/3 ote that the observed shape (=sub-type) of an elliptical galaxy depends on the aspect angle! lliptical Galaxies 6 D O D lliptical Galaxies X D S adial brightness distribution in ellipticals is given by de aucouleurs law: ( ) [ ( ) 1/4 () log = ] e e (17.1) where (): surface brightness, e.g., in pc 2 e: effective radius, i.e., radius containing in half of the total luminosity lliptical Galaxies 7

4 31 (Sb; ndromeda galaxy ), 90 (Sb), OO/U/S G 4565 (Sb, seen edge on), caughlin 51 (Sc), OO/U/S, T. ector

5 D Spiral Galaxies 51 (G 5194 and 5195), Sc and rr, Kitt Peak 0.9 m D SG X D Spiral Galaxies () e = " e 1/4 (17.2) 1 # () = 0 exp /0 ing in half of the total luminosity 10 (17.3) (): surface brightness, e.g., in pc 2 e: effective radius, i.e., radius contain- where log adial intensity profile: Bulge: de aucouleurs law (same as ellipticals!): Spiral Galaxies Spiral arms probably due to density wave. Gas content increases from Sa to Sc from 1% to 8%. ass content , with / 20, Bluer than ellipticals. Spiral Galaxies: lliptical nucleus ( bulge ) plus disk with spiral arms, designated Sa, Sb, Sc depending on opening angle of spiral (Sa: 10, Sc: 20 ) and dominance of nucleus. Spiral Galaxies where 0: scale length (typical, e.g., thin disk of ilky Way: 3 kpc) Disk: xponential law: O G 300 (Sc),. Schirmer/SO/2.2 m D SG X D 51 (Sc; center), HST/S D O

6 G 4921 (SBab; but note low star formation! HST/STSc) G 4921 (SBab; but note low star formation! HST/STSc) 58 (SBb), OO/U/S G 1365 (SBb, T/OS/TU): note old reddish bar, young spiral arms

7 D D SG X D Barred Galaxies 83 (SBc, SO) Barred Galaxies ilky Way is a barred spiral. Similar masses and gas content as in normal spirals (G 3351), SBb, T Barred Galaxies: lassification as SBa, SBb, SBc similar to Sx galaxies, but additional presence of a bar (cause of bar production and stability are still debated). O arge agellanic loud (; rr ), U/OO/S arge agellanic loud (; rr ), oke Kun Tan

8 D O D rregular Galaxies: rr X D S rr : asymmetrical and abnormal = ll objects that do not fit in the rest of the classification: starburst galaxies, interacting galaxies, Seyfert galaxies,... 82, HST-WP rregular Galaxies: rr 2 D O D aveats: Selection ffects X D S diameter: edge of a galaxy is not well defined as intensity decreases strongly from center. Wide range of observed radii: kpc (dwarf galaxies) to 30 kpc (normal spirals) and 50 kpc (ellipticals) ngular diameters depend on sky brightness Often used: D21 contour (= isophotal contour where galaxy becomes fainter than 21 mag arcsec 2 ) Small Galaxies can not be distinguished from stars ow surface brightness galaxies can not be seen against sky background. Karttunen aveats 1 D O D rregular Galaxies: rr X D S rr : no symmetry or spiral arms, bright knots of O- and B-type stars, very blue (B 0.5), high dust content ( 16%), / 3, masses vary appreciably from 10 6 to xamples: S, = agellanic type irregulars. G 4449, Univ. Bonn rregular Galaxies: rr 3 SO202-G23 (T UT1/S/SO)

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