3d spectrography v – density waves in the inner regions of galaxies
DESCRIPTION
3D spectrography V – Density waves in the inner regions of galaxies. D ensity W aves in galaxies. Warps. Spirals. > 50% of grand-design. All disk galaxies?. Lindblad, Lin & Shu (60’s). (Sancisi 76). Lopsidedness. Bars. > 70% of spirals?. Very common. (Kamphuis et al. 91). - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/1.jpg)
Padova 033D Spectrography
3D spectrography3D spectrography
V – Density waves in the innerV – Density waves in the inner
regions of galaxies regions of galaxies
![Page 2: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/2.jpg)
Padova 033D Spectrography
DDensity ensity WWaves in aves in galaxiesgalaxies
Spirals
Bars
> 50% of grand-design
> 70% of spirals?
Lindblad, Lin & Shu (60’s)
Warps
Lopsidedness
All disk galaxies?
Very common
(Kamphuis et al. 91)
(Sancisi 76)
![Page 3: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/3.jpg)
Padova 033D Spectrography
Role of Role of DDensity ensity WWavesaves
Torques Local density enhancements crowding,
shocks Angular momentum transfer Dynamical diffusion / heating
– Link with: Secular evolution?
Star formation, starbursts?– AGN?–
NGC 4314
![Page 4: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/4.jpg)
Padova 033D Spectrography
IDWIDW: Towards the centre: Towards the centre Shorter dynamical timescales !! Peaked density distributions (cusps, BHs) A priori lower fraction of dark matter (besides the BH), Axisymmetrisation? Importance of self-gravity
A few numbers:
100 pc 100 pc 10 1066 yrs at 100 km/s yrs at 100 km/s
• Duty cycle of an AGN? 107 – 108
yr
• Average Fueling rate? 0.001 – 1 Msun / yr
• Total mass used? 104-108 Msun
![Page 5: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/5.jpg)
Padova 033D Spectrography
Epicycles and resonancesEpicycles and resonances
Natural frequency of the system: angular frequency
For a disk (potential ):
RR
R
V
VRR
RRR
c
c
2c
z
V
Ω
L
2
0 0et0th Ordre
![Page 6: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/6.jpg)
Padova 033D Spectrography
Natural frequencies of the system:: circular frequency : radial epicyclic frequency
Epicycles and resonancesEpicycles and resonances
zzz
RRR
0
0
0
zz
Rt
RRR
02
2
0th Order
00
2
000
2
2
cos
03
00
tttRR
RR
RRRR
RzRR
zRR
For a disk (potential ):
![Page 7: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/7.jpg)
Padova 033D Spectrography
Rotating with an angular velocity
Epicycles and resonancesEpicycles and resonances
0
2
22
22
2
0
4
4
zRRz
ABBR
R
Natural frequencies of the system:: circular frequency : radial epicyclic frequency
For a disk (potential ):
![Page 8: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/8.jpg)
Padova 033D Spectrography
Epicycles and resonancesEpicycles and resonances
2:rotation Rigid
2:rotationFlat
:Keplerian
Natural frequencies of the system:: circular frequency : radial epicyclic frequency
For a disk (potential ):
![Page 9: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/9.jpg)
Padova 033D Spectrography
PrecessionPrecession
● Precession of elliptical orbits: / 2
Alignement Non Alignement
Structure with rigid rotation p if:
p / 2 = CTE
![Page 10: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/10.jpg)
Padova 033D Spectrography
Propagation, amplificationPropagation, amplification
CR
ILR
If Q > 1: evanescent waves
Potential is a superposition of spiral perturbations
j
jjjj RfmtitR exp,,
![Page 11: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/11.jpg)
Padova 033D Spectrography
Bars and angular Bars and angular momentummomentum
● Gas outside the CR
● Gas between the CR and l’ILR
OLR
ILR
Change of orientation of the orbits at the resonances :
gradual change for the gas
![Page 12: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/12.jpg)
Padova 033D Spectrography
NGC 1068NGC 1068
Lai (CFHT, I + K + Br
N E
![Page 13: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/13.jpg)
Padova 033D Spectrography
NGC 1068 with SAURONNGC 1068 with SAURON
NE
Coll.: K. Fathi, H. Wozniak, P. Ferruit, R. Peletier & the SAURON team
![Page 14: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/14.jpg)
Padova 033D Spectrography
Modelling NGC 1068Modelling NGC 1068
• Mass model: NIR Photometry and Velocity curve• Stars and gas: ‘’Ringberg standards’’
Coll.: K. Fathi, H. Wozniak, P. Ferruit, R. Peletier & the SAURON team
![Page 15: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/15.jpg)
Padova 033D Spectrography
Gas…Gas…
N E
Coll.: K. Fathi, H. Wozniak, P. Ferruit, R. Peletier & the SAURON team
Model
SAURON
![Page 16: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/16.jpg)
Padova 033D Spectrography
SAURON
Model
And stars…And stars…
N E
Coll.: K. Fathi, H. Wozniak, P. Ferruit, R. Peletier & the SAURON team
![Page 17: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/17.jpg)
Padova 033D Spectrography
IDWIDW: Inner bars versus AGN?: Inner bars versus AGN?
The DEBCA project
NGC 1808(starburst)
H band
Emsellem, Greusard, Combes et al. 01, A&A 368, 52
ISAAC / VLTCO bandhead (2.3 m)
SDD
major minor
![Page 18: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/18.jpg)
Padova 033D Spectrography
NGC 3623 (Sa)
Gnd based Image 7' x 7' Stars
SAURON / WHT
SStellartellar DDispersion ispersion DDroprops in 2Ds in 2D
![Page 19: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/19.jpg)
Padova 033D Spectrography
Nuclear spiralsNuclear spirals
Regan & Mulchaey 99, AJ 117, 2676 (HST, WFPC2 / NICMOS)
1.6 m100 pc
![Page 20: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/20.jpg)
Padova 033D Spectrography
IDWIDW: Inner spirals: Inner spirals
DSS 4’x4’
NGC 2974
E4 Vs = 1866 km/sD ~ 25 Mpc
Mdust ~ 1.5 106 Msun (IRAS)MHI ~ 8 108 Msun (Kim et al. 1988)MHII ~ 3 104 Msun (Buson et al. 1993)
Emsellem & Goudfrooij 03, MNRAS
![Page 21: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/21.jpg)
Padova 033D Spectrography
NGC 2974
E(V - I)
WFPC2
[NII]+H
240 pcLRF
Emsellem & Goudfrooij 03, MNRAS
IDWIDW: Inner spirals: Inner spirals
![Page 22: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/22.jpg)
Padova 033D Spectrography
And the winner is …And the winner is …
Emsellem & Goudfrooij 03, MNRAS
![Page 23: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/23.jpg)
Padova 033D Spectrography
The inner bar: Integral Field The inner bar: Integral Field datadata
NGC 2974
TIGER – CFHT(3D Deconvolution)
Emsellem & Goudfrooij 03, MNRAS
V
![Page 24: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/24.jpg)
Padova 033D Spectrography
NGC 3504NGC 3504: m=1 : m=1 modesmodes
NGC 3504
Optical
NIR
Combes et al.
PUEO / CFHT
WFPC2 / HST
OASIS / CFHT
I band
Coll.: Didier Greusard, Françoise Combes
arcsec
![Page 25: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/25.jpg)
Padova 033D Spectrography
PUEO/CFHT
WFPC2/HST
K
F606W
OASIS / CFHT
H [NII]
Vgas[OI]
NGC 3504
Coll.: Didier Greusard, Françoise Combes
NGC 3504NGC 3504: m=1 : m=1 modesmodes
![Page 26: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/26.jpg)
Padova 033D Spectrography
Berman 01, A&A 371, 476
gas flow model
Absorption map model
kpc
kpcar
csec
F814W
5 pc
arcsec
HRCAM
IDW: Towards the BH
M 31
STIS
Bulge & Nucleus
UV peak
Bacon, Emsellem, Monnet, et al. 1994, Emsellem & Combes 1997: Mbh = 7 107 Msun
![Page 27: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/27.jpg)
Padova 033D Spectrography
M31 – KepleriM31 – Kepleri an m=1an m=1
I V
OASIS / CFHT
N body simulation
Bacon, Emsellem, Combes, et al. 01, A&A 371, 409
![Page 28: 3D spectrography V – Density waves in the inner regions of galaxies](https://reader035.vdocuments.site/reader035/viewer/2022062809/5681598e550346895dc6d82f/html5/thumbnails/28.jpg)
Padova 033D Spectrography
Summary - ConclusionsSummary - Conclusions• Density waves have an important role in redistributing the
dissipative component and reshaping the galaxy (nuclear disks) Resonances!!
• Density waves are present in the central regions of galaxies. nuclear bars versus central starbursts (cold system) nuclear spirals are common but have low amplitudes … nuclear m=1 modes may be common keplerian m=1 (M 31)
• The presence of gas is critical
• 3D spectrography is required (again…)
• Central starburst – AGN: evolution sequence?
• Time-scales! (fueling the nucleus, starburst, AGN, dynamical heating …)