the evolution of stars and gas in galaxies phd thesis proposal philip lah
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![Page 1: The Evolution of Stars and Gas in Galaxies PhD Thesis Proposal Philip Lah](https://reader035.vdocuments.mx/reader035/viewer/2022070412/56649d585503460f94a3865c/html5/thumbnails/1.jpg)
The Evolution of Stars and Gas
in Galaxies
PhD Thesis Proposal
Philip Lah
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Supervisor: Frank Briggs
Supervisory Panel:
• Erwin de Blok (RSAA)
• Jayaram Chengalur (National Centre for Radio Astrophysics, India)
• Matthew Colless (Anglo-Australian Observatory)
• Roberto De Propris (University of Bristol, UK)
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Goal of PhD
• to relate the evolution in galaxies of their star formation rate, their stellar mass and their mass of neutral hydrogen gas (the fuel of star formation)
• examine galaxy evolution over last 4 Gyr (going back third age of the universe)
• study galaxies in a variety of different environments
• UNIQUE PART study galaxy properties in same systems – optically selected galaxies
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Why do this?
Should give a clearer picture of how, when and where stars and their host galaxies form.
Improves our understanding of our place in the universe, residing in our galaxy, the Milky Way, and orbiting our star, the Sun.
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Background
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Star Formation Rate
SubaruField
Hα Spectroscopy
Hα Narrow Band Imaging
UV (with no dust correction)
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Stellar Mass Density
Dickenson et al. 2003
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Neutral Hydrogen Gas Mass
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Neutral Hydrogen Gas Mass
HIPASSHI 21cm
Rao & Turnshek
2003
Storrie-Lombardi
& Wolfe 2000
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Galaxy Environment
galaxy environment cluster, cluster outskirts and the field
• density - morphology relation
• density - star formation relation
• density - neutral hydrogen relation
Cause of density relations?
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HI 21cm Emission at
High Redshift
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Previous highest redshift HI
Westerbork Synthesis Radio Telescope (WSRT)
Netherlands
Abell 2218 z = 0.18
integration time 36 days, Zwaan et al. 2001
Very Large Array (VLA)
Abell 2192 z = 0.1887
integration time ~80 hours, Veheijen et al. 2004
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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Giant Metrewave Radio Telescope
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GMRT Antenna Positions
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GMRT Collecting Area
30 dishes of 45 m diameter
GMRT Collecting Area
21 × ATCA
15 × Parkes
6.9 × WSRT
3.6 × VLA
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Method of HI Detection
• individual galaxies HI 21cm emission below radio observational detection limits
• large sample of galaxies with known positions & precise redshifts (from optical observations)
• coadd weak HI signals isolated in position & redshift (velocity) space
• measure integrated HI signal – total HI mass of whole galaxy population – can calculate the average HI galaxy mass
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Observational Targets
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Table of Targets
Target zLook Back Time
νHIGMRT Obs
Time
Subaru Field
0.24 2.8 Gyr 1142 MHz 90 hours
Abell 370 0.37 4.0 Gyr 1033 MHz 70 hours
Cl0024+1654 0.39 4.2 Gyr 1022 MHz18 + 45 hours
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Galaxy Cluster Abell 370
RA
DEC 27’ × 27’
Cluster Centre
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Galaxy Cluster Abell 370
RA
DEC ~3’ × 3’
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Abell 370 Data
• 42 literature redshifts for Abell 370 cluster members 33 are usable – large error in σz ≥ ± 300 kms-1 (from Soucail et al. 1988 )
• obtaining imaging data ESO 2.2m/WFI with VRI filters 34’ × 33’ (queue scheduled by Sept) use to select sample for spectroscopic follow-up
• using AF2/WYFFOS 4.2m William Herschel Telescope, La Palma (sometime in Oct to Dec) for redshifts and star formation rate from [OII]
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Radio Data Cube
RA
DEC
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Spectrum through Cubegalaxy redshift
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Spectrum around Redshiftgalaxy redshift
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Flux around Galaxy in Velocity Space
galaxy redshift
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HI Abell 370
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RMS decrease
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Mass HI
Assuming an optically thin neutral hydrogen cloud
1
2
1
236
kms
V
Mpc
d
mJy
S
zM
M LHI
MHI* = 6.2 ×109 M (Zwaan et al. 2003)
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Abell 370 HI Mass
No. Redshifts
HI Mass Upper Limit
(with 95% certainty)
33 8.0 × 109 M 1.3 MHI
*
Estimates:
100 2.5 × 109 M 0.42 MHI
*
300 1.7 × 109 M 0.28 MHI*
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Galaxy Cluster Cl0024+1654
RA
DEC 21’ × 21’
Cluster Centre
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Galaxy Cluster Cl0024+1654
RA
DEC ~1’ × 1’
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Cl0024+1654 Data
• HST imaging 2181 galaxies with morphologies of which 195 spectroscopically confirmed cluster members (Treu et al. 2003)
• Hα narrow band imaging with Subaru star formation rates (Kodama et al. 2004)
• 296 literature redshifts within HI frequency limits of the GMRT observation (Cszoke et al. 2001)
• estimated HI Mass Upper Limit similar to Abell 370: ~1.7 × 109 M
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Subaru Field
RA
DEC
24’ × 30’
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Subaru Field Redshifts
Subaru Filter
FWHM (120 Å)
GMRT HI Freq Range
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Subaru Field Redshifts
No. Redshifts
Estimated HI Mass Upper Limit
(with 95% certainty)
166 3.1 × 108 M 0.052 MHI
*
number of target Hα emitting galaxies = 347
number of galaxies with quality ≥ 3 redshifts = 183
number of galaxies in GMRT HI freq range = 166
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Past and Future Work
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Previous Workstarted PhD 1st March 2004
• Mar to mid-July 1st Three Month Project - preliminary work on reducing Abell 370 GMRT data - creating data reduction pipeline
• mid-July to Aug completed reduction of one sideband of the 7 days of data - prepared results for a GMRT telescope proposal for galaxy cluster Cl0024+1652
• Sept to mid-Nov 2nd Three Month Project - 6dFGS working with Robert Proctor and Duncan Forbes (Swinburne University) and Matthew Colless (AAO)
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Previous Work
• mid Nov to Dec Literature Review for Thesis Proposal
• Jan 2005 traveled to India for GMRT observations galaxy cluster Cl0024+1652
• beginning of March 5 nights 2dF AAT redshift observations of the Subaru Field
• have been working on adapting and revising data reduction code for all GMRT data sets – developing partially automated flagging of data
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Future Work
rest 2005:
• finish data reduction code
• reduce Subaru data and publish results
• reduce Cl0024+1652 data and publish results
• Abell 370 spectroscopic observations using AF2/WYFFOS 4.2m William Herschel Telescope, La Palma (sometime in Oct to Dec) – for redshifts and star formation rate from [OII]
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Future Work2006:
• beginning year finish reducing Abell 370 data and publish results
• once published Subaru results may go back to GMRT TAC for another sample of field galaxies
• other possibilities:
- obtain more redshifts for coadding particularly on the outskirts of the clusters
- stellar mass measurements using redshifts and additional near-infrared imaging
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Future Work
2007:
• first 6 months - finish write up thesis / finish off anything left over from previous years
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The End
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Additional Slides
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The UV Plane
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Abell 370 UV plane
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UV Plane
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GMRT Beam