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UNM 29-Oct04
Galaxy-Halo Gas Kinematic Connection at 0.3 < z < 1
Collaborators:Chris Churchill (NMSU)Chuck Steidel (Caltech)Alice Shapley (Princeton)Wal Sargent (Caltech)Michael Murphy (IoA)
Glenn Kacprzak(New Mexico State University)
UNM 29-Oct04
How do the kinematics of the stellar component reflect that of the halokinematics?
Do absorption properties depend on the orientation of the host galaxy?
Is there a connection between absorption properties and host galaxy morphology?
Toward Establishing Kinematic Detailed Connections…
Our ultimate goal is to better understand how early epoch galaxy halos are built and sustained: Mg II absorbers provide excellent laboratory.
UNM 29-Oct04
Steidel et al. (2002)
Pilot Study of Mg II Galaxy Halo & Stellar Kinematics
In 4/4 strong systems, the Mg II gas co-rotates with the galaxy
In one weak system the absorption is at the systemic velocity of the galaxy.
RESULTS
Need a sample of galaxies that have a wide range of morphologies and orientations.
UNM 29-Oct04
Velocity km s-1
Mg II 2796 Absorber/Galaxy Selection
UNM 29-Oct04
z = 0.550 z = 0.551
z = 0.640 z = 0.661
z = 0.374
z = 0.525
z = 0.787
z = 0.346
z = 0.442
z = 0.553
z = 0.888
z = 0.729
z = 0.418
z = 0.494
z = 0.591
z = 0.298
z = 0.888
z = 0.472
z = 0.368z = 0.317
z = 0.437
z = 0.891z = 0.798
z = 0.656
z = 0.851
5”
5”
z = 0.534
z = 0.524
z = 0.312 z = 0.313
z = 0.393
z = 0.948
z = 0.430
z = 0.752
z = 0.383
z = 0.702
Quasar is oriented downward
UNM 29-Oct04
Simard et al. (2002)
NE
Galaxy Models: GIM2D
HST Galaxies
Model Images
Residual Images
UNM 29-Oct04
LuminosityImpact parameterDisk inclinationPA wrt QSOBulge to Total ratioBulge effective radiusDisk scale lengthHalf light radiusMorphological asymmetries
Toward Establishing Kinematic Detailed Connections…
Equivalent widthDoublet ratioVelocity spreadVelocity asymmetryNumber of cloudsTotal column density
Galaxy Properties Absorption Properties
UNM 29-Oct04
QSO
Velocity
Inte
nsi
ty
PA = 45o i = 90o PA = 45o i = 60o PA = 0o i = 90o PA = N/A i = 0o
cos(PA)sin(i) = 0.61 cos(PA)sin(i) = 1.0 cos(PA)sin(i) = 0.0
Testing a Simple Model of Orientation and Position Angle
UNM 29-Oct04
No Orientation Correlation!
More detailed models are needed
UNM 29-Oct04
Barred Spiral Structure!
GIM2D: Galaxy Asymmetry
HST Image Model Model Residual
UNM 29-Oct04
Asymmetry & Absorption Strength
Galaxy asymmetry and Impact parameter are both important factors in determining the absorption strength.
3.2σ correlation.
This suggests past minor mergers or interactions influence the quantity and/or velocity dispersion of halo gas.
UNM 29-Oct04
3C.336 Field Absorbers & Non-Absorbers
UNM 29-Oct04
Absorbers vs. Non-Absorbers within 25΄΄
Possible techniques for finding absorbers in a galaxy rich field.
We will obtain photo-z this summer.
UNM 29-Oct04
• Halo gas is “aware” of the kinematics of the galaxy (pilot study 5 galaxies).
• There are no clear trends between absorption strength and orientation of the galaxy. More detailed models are needed.
• 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.
• Some indication that absorbers and non-absorbers may differ in their luminosity weighted morphological perturbations.
• Incorporate C IV and other ionization species into the analysis.
• Obtain redshifts of remaining candidates in order to increase sample size to over 50.
• Obtain rotation curves of the galaxy using Gemini and Keck.
• Obtain photometric redshifts of all HST fields to 200+kpc and fixed limiting absolute magnitude.
Conclusions …
Future …
UNM 29-Oct04
Forbidden Gas Lagging Halo
Ellison et al. (2003)
Swaters et al. (1997)Schaap et al. (2000)Sancisi et al. (2001)
Fraternali et al. (2002)
CAUTIONARY TAIL: A counter example!!
MC 1331+170; zabs=0.7446; Edge on spiral that does not align with disk kinematics! Because of the symmetric velocity splittings, this has been interpreted as superbubbles (Bond+ 2001; Ellison+ 2003).
UNM 29-Oct04 Observed spectra contain an admixture of both models
Asymmetric Blended Line Morphology
Symmetric Resolved Line Morphology
UNM 29-Oct04
Swaters et al. (1997)
Halo gas appears to rotate 25 to 100 km s-1 more slowly than the gas in the plane.
Disk gas
Halo gas
• D = 9.5 Mpc• Neutral hydrogen map from WSRT• Presence of an H I halo extending up
to at least 5 kpc from the plane
21-cm Mapping of Rotations Curves in Lower Halos…