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AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
Galaxy Properties vs Morphology
Galaxy Properties vs Morphology
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
JPH 76
JPH 76
Color vs Magnitude --- for Ellipticals less luminous galaxies are
Color vs Magnitude --- for Ellipticals less luminous galaxies are
SDSS (u-r) vs M Baldry et al 2004
SDSS (u-r) vs M Baldry et al 2004
SDSS
SDSS
Color Gradients --- most galaxies get bluer with radius
Color Gradients --- most galaxies get bluer with radius
De Vaucouleurs
De Vaucouleurs
HI content Type MH/M E 10-6  10-3 S0 0.005 Mort Sa 0.03 Roberts Sb 0
HI content Type MH/M E 10-6 10-3 S0 0.005 Mort Sa 0.03 Roberts Sb 0
Spirals HI vs T
Spirals HI vs T
Internal Motions
Internal Motions
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
NGC 253
NGC 253
M33 NRAO
M33 NRAO
Luminosity vs Internal Motions For Ellipticals, L vs
Luminosity vs Internal Motions For Ellipticals, L vs
K-Band TF
K-Band TF
Comparison of FJ & TF relations note the scatter
Comparison of FJ & TF relations note the scatter
Kinematics & Luminosity
Kinematics & Luminosity
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
The Fundamental Plane
The Fundamental Plane
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
Galaxy Spectra & SEDs
Galaxy Spectra & SEDs
Spectra
Spectra
M77 a.k.a. NGC1068
M77 a.k.a. NGC1068
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
Starburst
Starburst
The Cosmic Spectrum
The Cosmic Spectrum
Morphology Density Relation
Morphology Density Relation
<L> and color, too
<L> and color, too
Remember: Reading Assignment
Remember: Reading Assignment
Accepting suggestions What should we read next week
Accepting suggestions What should we read next week

: AY202a Galaxies Dynamics Lecture 3: Galaxy Characteristics. : John Huchra. : AY202a Galaxies Dynamics Lecture 3: Galaxy Characteristics.ppt. zip-: 2023 .

AY202a Galaxies Dynamics Lecture 3: Galaxy Characteristics

AY202a Galaxies Dynamics Lecture 3: Galaxy Characteristics.ppt
1 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics

AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics

2 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
3 Galaxy Properties vs Morphology

Galaxy Properties vs Morphology

Type vs Color This is essentially star formation rate and history B-V

U-B

cI Im-Sd Sc Sb Sa S0/a E/S0

blue

red

4 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
5 JPH 76

JPH 76

6 Color vs Magnitude --- for Ellipticals less luminous galaxies are

Color vs Magnitude --- for Ellipticals less luminous galaxies are

lower metallicity and thus bluer. CM for the Virgo Cluster from Visvanathan & Sandage (1978) Use as a distance indicator?

7 SDSS (u-r) vs M Baldry et al 2004

SDSS (u-r) vs M Baldry et al 2004

8 SDSS

SDSS

9 Color Gradients --- most galaxies get bluer with radius

Color Gradients --- most galaxies get bluer with radius

Combination of CFR + [Fe/H]

Liu, C-Z. et al. 2009, Research in Astron. Astrophys. X

10 De Vaucouleurs

De Vaucouleurs

11 HI content Type MH/M E 10-6  10-3 S0 0.005 Mort Sa 0.03 Roberts Sb 0

HI content Type MH/M E 10-6 10-3 S0 0.005 Mort Sa 0.03 Roberts Sb 0

05 Sc 0.1 Im 0.2 0.5

12 Spirals HI vs T

Spirals HI vs T

13 Internal Motions

Internal Motions

1970s improvements in detectors enabled research on several questions: 1. Do Es rotate appropriately? 2. Does ? vary with L? 3. Are Es triaxial? 4. Are Ss stable?

Theory

Data

Illingworth 1977

14 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
15 NGC 253

NGC 253

16 M33 NRAO

M33 NRAO

Optical Rotation Curves Radio 21-cm HI Velocity Maps

Bureau & Freeman

17 Luminosity vs Internal Motions For Ellipticals, L vs

Luminosity vs Internal Motions For Ellipticals, L vs

= Faber-Jackson For Spirals, L vs v = Tully-Fisher

TF 1977

FJ 1976

18 K-Band TF

K-Band TF

Masters et al. 2008

19 Comparison of FJ & TF relations note the scatter

Comparison of FJ & TF relations note the scatter

C. Kochanek

20 Kinematics & Luminosity

Kinematics & Luminosity

What drives the kinematics vs L relations? 1. Assume galaxies are self-similar in form <?(r)> ~ ?e 2. Assume they are made of similar stars M/L similar L ~ 4 ? Re 2 ?e where Re is the galaxys effective radius G m M / Re = ? m V2 circular orbits, flat rotation ? M ~ ? V2 R / G and Re = L? /(4 ? ?e)1/2 Thus M = ? V2 L? / (4 ? ?eG )1/2 = 1/4 V2 L? / (? ?eG )1/2 so for constant M/L , L? = 1/4 V2 / (? ?eG )1/2 or L ~ const V4 (shades of Opik)

)1/2

21 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
22 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
23 The Fundamental Plane

The Fundamental Plane

For E Galaxies, the combination of ? vs L + D vs L + ? vs L , if M/L is well behaved ? The Fundamental Plane (DD, 7 Sam) Re = f(?,L) or even better f(?,L,[Fe/H]) log Re = 0.36(<Ie> / ?B) + 1.4 log ?0 Ditto for Sprials. TF implication is that M/L varies by most a factor of 2 over a factor of 100 in Luminosity.

24 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
25 Galaxy Spectra & SEDs

Galaxy Spectra & SEDs

26 Spectra

Spectra

27 M77 a.k.a. NGC1068

M77 a.k.a. NGC1068

28 AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
29 Starburst

Starburst

30 The Cosmic Spectrum

The Cosmic Spectrum

Glazebrook & Baldry from the 250,000 2dF Galaxy Spectra

31 Morphology Density Relation

Morphology Density Relation

Dressler (1980) studied the gross morphologies of galaxies in 14 clusters.

32 <L> and color, too

<L> and color, too

SDSS

33 Remember: Reading Assignment

Remember: Reading Assignment

For this Wednesday NFW The Structure of Cold Dark Matter Halos, 1996, ApJ...463..563 & The preface to Zwickys Catalogue of Compact and Post-Eruptive Galaxies Read, Outline, be prepared to discuss Zwickys comments and the NFW profile.

34 Accepting suggestions What should we read next week

Accepting suggestions What should we read next week

Topic: Galactic Structure & Internal Dynamics

AY202a Galaxies Dynamics Lecture 3: Galaxy Characteristics
http://900igr.net/prezentacija/bez_uroka/ay202a-galaxies-dynamics-lecture-3-galaxy-characteristics-240117.html
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