26
Masses of Galaxy Groups Brent Tully University of Hawaii

Masses of Galaxy Groups Brent Tully University of Hawaii

Embed Size (px)

Citation preview

Page 1: Masses of Galaxy Groups Brent Tully University of Hawaii

Masses of Galaxy GroupsBrent TullyUniversity of Hawaii

Page 2: Masses of Galaxy Groups Brent Tully University of Hawaii

Masses of Galaxy GroupsBrent TullyUniversity of Hawaii

A galaxy group? What’s that?

Page 3: Masses of Galaxy Groups Brent Tully University of Hawaii

Considerations from theory

Spherical infall of cold, collisionless particles:

Radius

Velocity Radius

Time

r2t

r2t

- object at first turnaround today at t0 (radius r1t) will fully collapse by 2t0

- object at second turnaround today (radius r2t) was at first turnaround at 0.37 t0

Page 4: Masses of Galaxy Groups Brent Tully University of Hawaii

Useful observable manifestations of infall and caustics?

I. Mass - radius scaling relations

tcollapse ~ -1/2 ~ (r3/M) 1/2

Page 5: Masses of Galaxy Groups Brent Tully University of Hawaii

Useful observable manifestations of infall and caustics?

I. Mass - radius scaling relations

tcollapse ~ -1/2 ~ (r3/M) 1/2

For two structures at the same phase of collapse today:

r1 = r2 (M1/M2)1/3

r13/M1 = r2

3/M2

Page 6: Masses of Galaxy Groups Brent Tully University of Hawaii

Useful observable manifestations of infall and caustics?

I. Mass - radius scaling relations

tcollapse ~ -1/2 ~ (r3/M) 1/2

M ~ rms2 r2t

So at tcollapse = today r2t3 / rms

2 r2t = constant

rms ~ r2t

Page 7: Masses of Galaxy Groups Brent Tully University of Hawaii

Ωm in a flat universe

II. Manifestation of Dark Energy: almost no effect on relation between mass and 2nd turnaround radius r 2t

but affects the rate of the development of structure so affects the relation between 1st and 2nd turnaround r1t / r2t

Page 8: Masses of Galaxy Groups Brent Tully University of Hawaii

Observations of the caustic of second turnaround (radius r2t)

NGC 5846 Group

Distance = 26 Mpc

3rd largest knot of E/S0galaxies within thisdistance, after Virgo, Fornax

rms = 322 km/s (85 veloc.)r2t = 840 kpcM = 8 1013 M

Large dE population

(325 candidate members)

Page 9: Masses of Galaxy Groups Brent Tully University of Hawaii

Caustic of 2nd turnaround in N5846 group (continued)

rms = 322 km/s

r2t = 840 kpc

Page 10: Masses of Galaxy Groups Brent Tully University of Hawaii

NGC 5353/4 Group mass = 2.1 1013 suns

rms = 205 km/s

r2t = 530 kpc

Page 11: Masses of Galaxy Groups Brent Tully University of Hawaii

NGC 1023 Group

mass = 6.4 1012 sunsrms = 136 km/s

r2t = 350 kpc

Page 12: Masses of Galaxy Groups Brent Tully University of Hawaii

Virgo region

Page 13: Masses of Galaxy Groups Brent Tully University of Hawaii

Virgo Cluster

Vrms = 715 km/sR2t = 1.96 MpcM = 9 1014 M

Page 14: Masses of Galaxy Groups Brent Tully University of Hawaii

Virgo region

M > 9 1014 M

Page 15: Masses of Galaxy Groups Brent Tully University of Hawaii

Caustic of 2nd turnaround r2t correlations

Red: results from wide field imaging with CFHT MegaCam N5846: Mahdavi et al. 2005, AJ, 130, 1502

N1407: Trentham et al. 2006, MNRAS, 369, 1375

N5353/4: Tully & Trentham 2008, AJ, 135, 1488

N1023: Trentham & Tully 2009, MNRAS, in press

M81: Chiboucas et al. 2009, AJ, 137, 3009

Page 16: Masses of Galaxy Groups Brent Tully University of Hawaii

Caustic of 2nd turnaround r2t correlations

r2t = v/390 = 0.193 (M12)1/3 ==> M12 = 2.3 10-6 v3

virial mass within r2t (units 1012 M)1D rms velocity dispersion of galaxies within r2t

Page 17: Masses of Galaxy Groups Brent Tully University of Hawaii

Correlation between group mass and dwarf population!

No. dwarfs per unit parent halo mass ~ constant

Fewer giants per unit parent halo mass in more dynamically evolved halos

dwarf: -17 < MR < -11 giant: MR < -17

Page 18: Masses of Galaxy Groups Brent Tully University of Hawaii

Correlation between group mass and dwarf population!

No. dwarfs per unit parent halo mass ~ constant

Fewer giants per unit parent halo mass in more dynamically evolved halos

evolved groups

spiral groups

dwarf associations

dwarf: -17 < MR < -11 giant: MR < -17

Page 19: Masses of Galaxy Groups Brent Tully University of Hawaii

Local Group

Mmw ~ Mm31 ~ 1 1012 M

=> r2t ~ 200 kpc

Page 20: Masses of Galaxy Groups Brent Tully University of Hawaii

Local Group (continued)

r2t r1t

r1t = 960 kpcMT(LG) = 1.9 1012 M

Page 21: Masses of Galaxy Groups Brent Tully University of Hawaii

Virgo zero velocity surface~ 7 Mpc radius

Page 22: Masses of Galaxy Groups Brent Tully University of Hawaii

The Local Sheetred circles: 2nd turnaround r2t

blue circles: zero velocity r1t

Page 23: Masses of Galaxy Groups Brent Tully University of Hawaii

The Local Sheetred circles: 2nd turnaround r2t

blue circles: zero velocity r1t

green circles: zero gravity surface (=0.7, spherical infall, no angular momentum)

Page 24: Masses of Galaxy Groups Brent Tully University of Hawaii

Summary

Light to mass varies with environmentLB = 3.25 1010 M12

.59 e-(0.6/M12

)

Observed caustic of 2nd turnaroundstrongly correlated with virial massr2t = 0.193 (M12)1/3 Mpc

and with velocity dispersioninterior to 2nd turnaroundr2t = v / 390 Mpc

mass of parent halo

M12 = 2.3 10-6 v3

Page 25: Masses of Galaxy Groups Brent Tully University of Hawaii

Summary

Light to mass varies with environmentLB = 3.25 1010 M12

.59 e-(0.6/M12

)

Observed caustic of 2nd turnaroundstrongly correlated with virial massr2t = 0.193 (M12)1/3 Mpc

and with velocity dispersioninterior to 2nd turnaroundr2t = v / 390 Mpc

mass of parent halo

M12 = 2.3 10-6 v3

No. dwarfs correlated with halo mass

Nd ~ M.91

dynamically evolved

spiral rich

Page 26: Masses of Galaxy Groups Brent Tully University of Hawaii

Summary

Light to mass varies with environmentLB = 3.25 1010 M12

.59 e-(0.6/M12

)

Observed caustic of 2nd turnaroundstrongly correlated with virial massr2t = 0.193 (M12)1/3 Mpc

and with velocity dispersioninterior to 2nd turnaroundr2t = v / 390 Mpc

mass of parent halo

M12 = 2.3 10-6 v3

No. dwarfs correlated with halo mass

Nd ~ M.91

dynamically evolved

spiral rich

signatures of dark energyIf = 0.7 r1t ~ 3.3 r2t (3.7 r2t if = 0) and rZG~ 1.4 r1t