Download G. Kacprzak "Galaxy-halo and gas connection 0.5 email

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Study Mg II quasar absorption line systems in order to understand
the kinematics of halos probing distances out to 70 kpcs from the
galaxies.
Therefore the galaxies in our sample are selected by the known
presence of Mg II absorption
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Determine whether the galaxy kinematics and/or morphologies are
coupled to the halo kinematics
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Our main goal is to determine how early epoch galaxy halos are
built and sustained.
Mg II 2796, 2803
2796
2803
Mg II 2796, 2803
Velocity km s-1
Sample includes absorbers with W(2796) < 1
Selected 5 edge-on galaxies
4 of the 5 showed the trend
for the halo gas kinematics
follows that of the galaxies
What is needed is a larger
sample which represents a
broad range of orientations
with respect to the quasar
line of sight
Steidel et al. (2002)
5”
z = 0.298
5”
z = 0.317
z = 0.346
z = 0.368
z = 0.374
Orientated such that the QSO is down
z = 0.418
z = 0.437
z = 0.442
z = 0.472
z = 0.494
z = 0.525
z = 0.550
z = 0.551
z = 0.553
z = 0.591
z = 0.640
z = 0.656
z = 0.661
z = 0.729
z = 0.787
z = 0.797
z = 0.851
z = 0.888
z = 0.888
z = 0.891
o
o
PA = 45 i = 0
o
o
PA = 45 i = 30
cos(PA)cos(i) = 0.61
o
o
PA = 0 i = 0
cos(PA)cos(i) = 1.0
Intensity
QSO
Velocity
o
PA = N/A i = 90
cos(PA)cos(i) = 0.0
“Normal” Absorbers
Wind Dominate & DLA Systems
z = 0.298
z = 0.317
z = 0.346
z = 0.368
z = 0.374
z = 0.418
z = 0.437
z = 0.442
z = 0.472
z = 0.494
z = 0.525
z = 0.550
z = 0.551
z = 0.553
z = 0.591
z = 0.640
z = 0.656
z = 0.661
z = 0.729
z = 0.787
z = 0.797
z = 0.851
z = 0.888
z = 0.888
z = 0.891
Simard et al. (2002)
N
E
HST Image
Model
RA32
> 0.05
RT
Model Residual
Barred Spiral Structure!
If more than 5% of the galaxies total residual flux is
due to asymmetries then these galaxies are
considered to not be “normal”; they are “asymmetric”.
Schade et al. (1995)
Asymmetric Galaxies
Wind Dominate & DLA Systems
“Normal” Galaxies
“Normal” Absorbers
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Halo gas is “aware” of the kinematics of the galaxy (pilot study 5
galaxies).
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There are no clear trends between absorption strength and
orientation of the galaxy. More detailed models are needed.
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Minor morphological perturbations are correlated to absorption
strength. This may suggest that most Mg II absorption selected
galaxies have had some previous minor interactions or
harassments.
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21 of 25 Keck HIRES spectra are in hand and are currently being
analyzed. The remaining quasar spectra will be obtained in the
near future.
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Obtain redshifts of remaining candidates in order to increase
sample size to over 50.
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Obtain rotation curves of the galaxy using Gemini and Keck.