nigel douglas university of groningen nigel douglas university of groningen measuring kinematics in...
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nigel douglas university of groningennigel douglas university of groningen
measuring kinematics in elliptical galaxiesmeasuring kinematics in elliptical galaxies
(spiral) galaxy dynamics
(spiral) galaxy dynamics
neutral gas
(stars, HII regions)
Braun 2002
rotation curve decomposition rotation curve decomposition
RotCurve (cwru.edu)RotCurve (cwru.edu)
early-type galaxy dynamics early-type galaxy dynamics stellar spectroscopy
Statler et al 99
IFU (integral field unit)
IFU (integral field unit)
Oosterloo priv comm
discrete tracers of kinematics
discrete tracers of kinematics
• globular clusters
• satellites
• PNe
• stars
• globular clusters
• satellites
• PNe
• stars
stellar streamsstellar streams
Ibata et al. 2004Ibata et al. 2004
PNe • easy to detect
• easy to measure radial velocity
linewidth 21 km/s
• ubiquitous at 2.5 20 per 109 LB
e.g. 750 for NGC 3379
PNe v stars
• by assumption PNe follow stars
• how true is this?
• PNe age and population synthesis
techniques for acquiring PNe radial velocities:
techniques for acquiring PNe radial velocities:
• imaging+spectroscopy
• perot-fabry
• slitless spectroscopy
imaging + spectroscopyngc 5128
Hui, Ford, Ciardullo, Jacoby 1993Hui, Ford, Freeman, Dopita 1995Peng, Ford, Freeman 2004
fabry-perot ngc 3384
fabry-perot ngc 3384
Tremblay, Merritt, Wiilliams 1995
68 PNe68 PNe
slitless spectroscopy:the PN spectrum
Slitless spectroscopy(1)Slitless spectroscopy(1)
trials at AAT 1995trials at AAT 1995
slitless spectroscopy NGC 5128 slitless spectroscopy NGC 5128
Slitless spectroscopy(2)Slitless spectroscopy(2)
cf Hui et al 1995
24 PNe compared
cf Hui et al 1995
24 PNe compared
Slitless spectroscopy(3)Slitless spectroscopy(3)
Fehrenbach 1947
Douglas & Taylor 1999
Fehrenbach 1947
Douglas & Taylor 1999
CDI at WHT: M94
modified ISIS
1997-2001
NGC 7457
NGC 5866
Douglas et al. 2000
MB = -19.8
D = 10.5 Mpc
UT1 + FORS1
1999/2000
14 hrs:
535 PN to 3 Reff
CDI at VLT: NGC 4697
Méndez et al. 2001
Bibliography: PNe velocitieswith slitless spectroscopy
Bibliography: PNe velocitieswith slitless spectroscopy
CDI (rotating spectrograph):
Douglas & Taylor 1999
Douglas, Gerssen et al 2000
CDI (mirror and grism):
Méndez, Riffeser et al 2001
PN.S (simultaneous CDI):
Douglas, Arnaboldi et al 2002
Romanowsky, Douglas et al 2003
CDI (rotating spectrograph):
Douglas & Taylor 1999
Douglas, Gerssen et al 2000
CDI (mirror and grism):
Méndez, Riffeser et al 2001
PN.S (simultaneous CDI):
Douglas, Arnaboldi et al 2002
Romanowsky, Douglas et al 2003
PN.S design
PN.S grating
PN.S mask
• instrument efficiency = 72% total system efficiency = 33%
three 36 Å [O III] filters ( -1400 .. +3400 km/s)
• field of view = 11.4’ x 10.3’ • dispersion 1.29 pxl/Å • built by prime optics, RSAA, ASTRON
Douglas et al 2002Douglas et al 2002
sample data
5’ x 2’ field in M31 (H. Merrett et al.)
pn.spectrograph projectpn.spectrograph project
pn.s team:
n. douglas, n. napolitano (groningen)
k. kuijken (leiden)
a. romanowsky, m. merrifield,
h. merrett (nottingham)
m. arnaboldi (turin)
m. capaccioli (naples)
k. freeman (rsaa)
o. gerhard (basel)
pn.s team:
n. douglas, n. napolitano (groningen)
k. kuijken (leiden)
a. romanowsky, m. merrifield,
h. merrett (nottingham)
m. arnaboldi (turin)
m. capaccioli (naples)
k. freeman (rsaa)
o. gerhard (basel)
sample of 12 bright, round E galaxies:
B 12.5, E2 or rounder,
v < 1300 km/s
100 - 400 PNe per galaxy, to 5-15 Reff
~ 8 hours to reach m5007 = 28.0
PN.S programme
WHT+PN.S:
March 2002
3 hrs :
197 PN velocities
to 7 Reff ,
v = 20 km/s
E1 , MB = -20.0
D = 11 Mpc
NGC 3379
Surface brightness profiles
PNe
stars(Capaccioli et al. 1990)
NGC 3379: Dispersion profile
isotropic constant-M/L Hernquist model
110 PNe
Isotropic singular isothermal halo
197 PNe
long-slit data(Statler & Smecker-Hane 1999)
29 PNe (Ciardullo, Jacoby & Dejonghe 1993)
Sluis et al. also confirmed with ~60 PNe
“Science three” dispersion profiles
isotropic
constant-M/L
Hernquist model
Romanowsky et al. 2003
(refs for long-slit:
Bender et al 1994)
Romanowsky et al. 2003
(refs for long-slit:
Bender et al 1994)
- single wavelength:
poor discrimination
utilises 0.1% of spectrum
+ undispersed H-alpha camera
PN.S limitations
M-CDI: masked counter-dispersed imaging
M-CDI: masked counter-dispersed imaging
past narrow band surveys at D > 10 Mpc: poor returns in follow-up spectroscopy
apply counter-dispersed imaging
(don’t need good astrometry)
but utilise all information
Ciardullo et al. 1998
UT2+FORS2/MXU:28-30 Apr 2001
MCDI
1400B VPH grism
6 fields @ 1 hr each:
200 PN velocities
to 5 Reff ,
v =15 km/s
PNe in M87
NGC3377
future developments:
NGC3377
future developments:
wavelength tagging detectors
NGC3377
future developments:
spectrum of an entire galaxy
NGC3377
future developments:
non-radial velocities