HI in Galaxies at Redshifts 0.1 to 1.0: Current and Future Observations Using Optical Redshifts for...
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Transcript of HI in Galaxies at Redshifts 0.1 to 1.0: Current and Future Observations Using Optical Redshifts for...
HI in Galaxies at Redshifts 0.1 to 1.0: Current and Future Observations
Using Optical Redshifts for HI Coadding
Melbourne 2008
Philip Lah
Collaborators:
Michael Pracy (ANU)
Frank Briggs (ANU)
Jayaram Chengalur (NCRA)
Matthew Colless (AAO)
Roberto De Propris (CTIO)
Talk OutlineIntroduction• Evolution in clusters & star formation rate density vs z• HI 21cm emission & the HI coadding technique
Current Observations with the HI coadding technique• HI in star forming galaxies at z = 0.24 • HI in Abell 370, a galaxy cluster at z = 0.37
Future Observations with SKA pathfinders• using ASKAP and WiggleZ• using MeerKAT and zCOSMOS
Evolution in Galaxy Clusters
Galaxy Cluster: Coma
Butcher-Oemler Effect
The Cosmic Star Formation Rate
Density
SFRD vs z
Hopkins 2004
SFRD vs time
Hopkins 2004
HI Gas and Star Formation
Neutral atomic hydrogen gas
cloud (HI)
molecular gas cloud (H
2)
star formation
The Cosmic
Neutral GasDensity
The Cosmic Gas Density vs. Redshift
Zwaan et al. 2005HIPASSHI 21cm
Rao et al.2006DLAs
from MgII absorption
Prochaskaet al. 2005
DLAs
The Cosmic Gas Density vs. Redshift
Zwaan et al. 2005HIPASSHI 21cm
Rao et al.2006DLAs
from MgII absorption
Prochaskaet al. 2005
DLAs
HI 21 cm Emission
Neutral atomic hydrogen creates 21 cm radiation
proton electron
Neutral atomic hydrogen creates 21 cm radiation
Neutral atomic hydrogen creates 21 cm radiation
Neutral atomic hydrogen creates 21 cm radiation
Neutral atomic hydrogen creates 21 cm radiation
photon
Neutral atomic hydrogen creates 21 cm radiation
HI 21cm emissionHI 21 cm emission decay half life ~10 million years (31014 s)
• 1 M 2.0 1033g 1.2 1057 atoms of hydrogen atoms
• total HI gas in galaxies ~ 107 to 1010 M
• HI emission ~4 1049 to 4 1052 photons per second
• HI 21 cm luminosity of ~4 1033 to 4 1036 ergs s-1
For comparison, in star forming galaxies:
• luminosity of H emission ~3 1039 to 3 1042 ergs s-1
HI 21 cm emission ~106 times less power than H emission
HI 21cm emissionHI 21 cm emission decay half life ~10 million years (31014 s)
• 1 M 2.0 1033g 1.2 1057 atoms of hydrogen atoms
• total HI gas in galaxies ~ 107 to 1010 M
• HI emission ~4 1049 to 4 1052 photons per second
• HI 21 cm luminosity of ~4 1033 to 4 1036 ergs s-1
For comparison, in star forming galaxies:
• luminosity of H emission ~3 1039 to 3 1042 ergs s-1
HI 21 cm emission ~106 times less power than H emission
HI 21cm emissionHI 21 cm emission decay half life ~10 million years (31014 s)
• 1 M 2.0 1033g 1.2 1057 atoms of hydrogen atoms
• total HI gas in galaxies ~ 107 to 1010 M
• HI emission ~4 1049 to 4 1052 photons per second
• HI 21 cm luminosity of ~4 1033 to 4 1036 ergs s-1
For comparison, in star forming galaxies:
• luminosity of H emission ~3 1039 to 3 1042 ergs s-1
HI 21 cm emission ~106 times less power than H emission
HI 21cm emissionHI 21 cm emission decay half life ~10 million years (31014 s)
• 1 M 2.0 1033g 1.2 1057 atoms of hydrogen atoms
• total HI gas in galaxies ~ 107 to 1010 M
• HI emission ~4 1049 to 4 1052 photons per second
• HI 21 cm luminosity of ~4 1033 to 4 1036 ergs s-1
For comparison, in star forming galaxies:
• luminosity of H emission ~3 1039 to 3 1042 ergs s-1
HI 21 cm emission ~106 times less power than H emission
HI 21cm emissionHI 21 cm emission decay half life ~10 million years (31014 s)
• 1 M 2.0 1033g 1.2 1057 atoms of hydrogen atoms
• total HI gas in galaxies ~ 107 to 1010 M
• HI emission ~4 1049 to 4 1052 photons per second
• HI 21 cm luminosity of ~4 1033 to 4 1036 ergs s-1
For comparison, in star forming galaxies:
• luminosity of H emission ~3 1039 to 3 1042 ergs s-1
HI 21 cm emission ~106 times less power than H emission
HI 21cm emissionHI 21 cm emission decay half life ~10 million years (31014 s)
• 1 M 2.0 1033g 1.2 1057 atoms of hydrogen atoms
• total HI gas in galaxies ~ 107 to 1010 M
• HI emission ~4 1049 to 4 1052 photons per second
• HI 21 cm luminosity of ~4 1033 to 4 1036 ergs s-1
For comparison, in star forming galaxies:
• luminosity of H emission ~3 1039 to 3 1042 ergs s-1
HI 21 cm emission ~106 times less power than H emission
HI 21cm emissionHI 21 cm emission decay half life ~10 million years (31014 s)
• 1 M 2.0 1033g 1.2 1057 atoms of hydrogen atoms
• total HI gas in galaxies ~ 107 to 1010 M
• HI emission ~4 1049 to 4 1052 photons per second
• HI 21 cm luminosity of ~4 1033 to 4 1036 ergs s-1
For comparison, in star forming galaxies:
• luminosity of H emission ~3 1039 to 3 1042 ergs s-1
HI 21 cm emission ~106 times less power than H emission
HI 21cm Emission at
High Redshift
HI 21cm emission at z > 0.1• single galaxy at z = 0.176 WSRT 200 hours (Zwaan
et al. 2001, Science, 293, 1800)
• single galaxy at z = 0.1887 VLA ~80 hours
(Verheijen et al. 2004,in IAU Symposium Vol 195, p. 394)
• two galaxy clusters at z = 0.188 and z = 0.206 WSRT 420 hours
42 galaxies detected HI gas masses 5109 to 41010 M
(Verheijen et al. 2007, ApJL, 668, L9)
• galaxies with redshifts z = 0.17 to 0.25 observed with Arecibo
detected 26 from 33 observed HI gas masses (2 to 6) 1010 M
(Catinella et al. 2007, in IAU Symposium Vol 235, p. 39)
HI 21cm emission at z > 0.1• single galaxy at z = 0.176 WSRT 200 hours (Zwaan
et al. 2001, Science, 293, 1800)
• single galaxy at z = 0.1887 VLA ~80 hours
(Verheijen et al. 2004,in IAU Symposium Vol 195, p. 394)
• two galaxy clusters at z = 0.188 and z = 0.206 WSRT 420 hours
42 galaxies detected HI gas masses 5109 to 41010 M
(Verheijen et al. 2007, ApJL, 668, L9)
• galaxies with redshifts z = 0.17 to 0.25 observed with Arecibo
detected 26 from 33 observed HI gas masses (2 to 6) 1010 M
(Catinella et al. 2007, in IAU Symposium Vol 235, p. 39)
HI 21cm emission at z > 0.1• single galaxy at z = 0.176 WSRT 200 hours (Zwaan
et al. 2001, Science, 293, 1800)
• single galaxy at z = 0.1887 VLA ~80 hours
(Verheijen et al. 2004,in IAU Symposium Vol 195, p. 394)
• two galaxy clusters at z = 0.188 and z = 0.206 WSRT 420 hours
42 galaxies detected HI gas masses 5109 to 41010 M
(Verheijen et al. 2007, ApJL, 668, L9)
• galaxies with redshifts z = 0.17 to 0.25 observed with Arecibo
detected 26 from 33 observed HI gas masses (2 to 6) 1010 M
(Catinella et al. 2007, in IAU Symposium Vol 235, p. 39)
HI 21cm emission at z > 0.1• single galaxy at z = 0.176 WSRT 200 hours (Zwaan
et al. 2001, Science, 293, 1800)
• single galaxy at z = 0.1887 VLA ~80 hours
(Verheijen et al. 2004,in IAU Symposium Vol 195, p. 394)
• two galaxy clusters at z = 0.188 and z = 0.206 WSRT 420 hours
42 galaxies detected HI gas masses 5109 to 41010 M
(Verheijen et al. 2007, ApJL, 668, L9)
• galaxies with redshifts z = 0.17 to 0.25 observed with Arecibo
detected 26 from 33 observed HI gas masses (2 to 6) 1010 M
(Catinella et al. 2007, in IAU Symposium Vol 235, p. 39)
Coadding HI signals
Coadding HI signals
RA
DEC
Radio Data Cube
Frequen
cy
HI red
shift
Coadding HI signals
RA
DEC
Radio Data Cube
Frequen
cy
HI red
shift
positions of optical galaxies
Coadding HI signals
frequency
flux
Coadding HI signals
frequency
flux
z2
z1
z3
Coadding HI signals
frequency
flux
z2
z1
z3 velocity
HI signal
Current Observations -HI coadding
Giant Metrewave Radio Telescope
Giant Metrewave Radio Telescope
Giant Metrewave Radio Telescope
Anglo-Australian Telescope
multi-object, fibre fedspectrograph
2dF/AAOmega instrument
The Fujita galaxies H emission galaxies at z = 0.24
The Subaru Telescope
The Surprime-cam filters
H atz = 0.24
Narrowband Filter: Hα detection
The Fujita Galaxies
Subaru Field 24’ × 30’
narrow band imaging Hα emission at z = 0.24
(Fujita et al. 2003, ApJL, 586, L115)
348 Fujita galaxies
121 redshifts using AAT
GMRT ~48 hours on field
DEC
RA
SFRD vs z - Fujita
Hopkins 2004
Fujita et al. 2003
Fujita galaxies - B filter
Thumbnails 10’’ sq
Ordered by H
luminosity
Fujita galaxies - B filter
Thumbnails 10’’ sq
Ordered by H
luminosity
Coadded HI
Spectrum
HI spectrum all
Fujita galaxies neutral hydrogen gas measurement
using 121 redshifts - weighted average
MHI = (2.26 ± 0.90) ×109 M
raw
binned
The Cosmic
Neutral GasDensity
my new point
The Cosmic Gas Density vs. Redshift
my new point
Cosmic Neutral Gas Density vs. Time
Galaxy HI mass vs
Star Formation Rate
Galaxy HI Mass vs Star Formation Rate
HIPASS&
IRASdataz ~ 0
Doyle & Drinkwater
2006
HI Mass vs Star Formation Rate at z = 0.24
line from Doyle &
Drinkwater 2006
all 121 galaxies
HI Mass vs Star Formation Rate at z = 0.24
line from Doyle &
Drinkwater 2006
42 bright L(Hα)
galaxies
42 medium L(Hα)
galaxies
37 faint L(Hα)
galaxies
Abell 370 a galaxy cluster at z = 0.37
Abell 370, a galaxy cluster at z = 0.37
large galaxy cluster of
order same size as
Coma
optical imaging ANU
40 inch telescope
spectroscopic follow-
up with the AAT
GMRT ~34 hours on
cluster
Abell 370 – R band imagesThumbnails
10’’ sq
324 galaxies with useful
redshifts (z~0.37)
Ordered by observed
R band magnitudes
Abell 370 galaxy cluster
324 galaxies
105 blue (B-V 0.57)
219 red (B-V > 0.57)
Abell 370 galaxy cluster
Abell 370 galaxy clusterAbell 370 galaxy cluster
3σ extent of X-ray gas
R200 radius at which cluster
200 times denser than the
general field
Galaxy Sizes
I want galaxies to be unresolved. For the Fujita galaxies I
used an estimate of the HI size from the optical properties of
spiral and irregular field galaxies and the smoothed radio
data.
Major Complication!!The Abell 370 galaxies are a mixture of early and late types
in a variety of environments.
Galaxy Sizes
I want galaxies to be unresolved. For the Fujita galaxies I
used an estimate of the HI size from the optical properties of
spiral and irregular field galaxies and the smoothed radio
data.
Major Complication!!The Abell 370 galaxies are a mixture of early and late types
in a variety of environments.
HI mass324 galaxies
219 galaxies
105 galaxies
94 galaxies
168 galaxies
156 galaxies
104 galaxies
220 galaxies
HI mass324 galaxies
219 galaxies
105 galaxies
94 galaxies
168 galaxies
156 galaxies
104 galaxies
220 galaxies
HI mass324 galaxies
219 galaxies
105 galaxies
94 galaxies
168 galaxies
156 galaxies
104 galaxies
220 galaxies
HI mass324 galaxies
219 galaxies
105 galaxies
94 galaxies
168 galaxies
156 galaxies
104 galaxies
220 galaxies
HI mass324 galaxies
219 galaxies
105 galaxies
94 galaxies
168 galaxies
156 galaxies
104 galaxies
220 galaxies
HI all spectrumall Abell 370 galaxies
neutral hydrogen gas measurement
using 324 redshifts – large smoothing
MHI = (6.6 ± 3.5) ×109 M
HI Flux – All Galaxies
HI blue outside x-ray gasblue galaxies
outside of x-ray gas measurement of neutral hydrogen
gas content
using 94 redshifts – large smoothing
MHI = (23.0 ± 7.7) ×109 M
HI Flux – Blue Galaxies Outside X-ray Gas
Comparisons with the
Literature
Average HI Mass Comparisons with
Coma
Abell 370 and Coma Comparison
220 galaxies
324 galaxies
104 galaxies
Abell 370 and Coma Comparison
220 galaxies
324 galaxies
104 galaxies
Abell 370 and Coma Comparison
220 galaxies
324 galaxies
104 galaxies
HI Density Comparisons
HI density field
HI density field
HI density field
HI density field
HI density - inner regions of clusters
within 2.5 Mpc of cluster centers
HI Mass to Light Ratios
HI Mass to Light Ratios
HI mass to optical B band luminosity for
Abell 370 galaxies
Uppsala General Catalog
Local Super Cluster
(Roberts & Haynes 1994)
HI Mass to Light Ratios
HI mass to optical B band luminosity for
Abell 370 galaxies
Uppsala General Catalog
Local Super Cluster
(Roberts & Haynes 1994)
Galaxy HI mass vs
Star Formation Rate
Galaxy HI Mass vs Star Formation Rate
HIPASS&
IRASdataz ~ 0
Doyle & Drinkwater
2006
HI Mass vs Star Formation Rate in Abell 370
all 168 [OII]
emission galaxies
line from Doyle &
Drinkwater 2006
HI Mass vs Star Formation Rate in Abell 370
84 blue [OII]
emission galaxies
line from Doyle &
Drinkwater 200692 red [OII]
emission galaxies
Future Observations -HI coadding
ASKAP
MeerKAT
South African SKA pathfinder
ASKAP and MeerKAT parametersASKAP MeerKAT
Number of Dishes 45 80
Dish Diameter 12 m 12 m
Aperture Efficiency 0.8 0.8
System Temp. 35 K 30 K
Frequency range 700 – 1800 MHz 700 – 10000 MHz
Instantaneous bandwidth 300 MHz 512 MHz
Field of View:
at 1420 MHz (z = 0)
at 700 MHz (z = 1)
30 deg2
30 deg2
1.2 deg2
4.8 deg2
Maximum Baseline Length 8 km 10 km
ASKAP and MeerKAT parametersASKAP MeerKAT
Number of Dishes 45 80
Dish Diameter 12 m 12 m
Aperture Efficiency 0.8 0.8
System Temp. 35 K 30 K
Frequency range 700 – 1800 MHz 700 – 10000 MHz
Instantaneous bandwidth 300 MHz 512 MHz
Field of View:
at 1420 MHz (z = 0)
at 700 MHz (z = 1)
30 deg2
30 deg2
1.2 deg2
4.8 deg2
Maximum Baseline Length 8 km 10 km
ASKAP and MeerKAT parametersASKAP MeerKAT
Number of Dishes 45 80
Dish Diameter 12 m 12 m
Aperture Efficiency 0.8 0.8
System Temp. 35 K 30 K
Frequency range 700 – 1800 MHz 700 – 10000 MHz
Instantaneous bandwidth 300 MHz 512 MHz
Field of View:
at 1420 MHz (z = 0)
at 700 MHz (z = 1)
30 deg2
30 deg2
1.2 deg2
4.8 deg2
Maximum Baseline Length 8 km 10 km
z = 0.4 to 1.0 in a single observation
z = 0.2 to 1.0 in a single observation
HI detections ASKAP 100 hr
HI detections ASKAP 1000 hr
HI detections MeerKAT 100 hr
HI detections MeerKAT 1000 hr
What I could do with
the SKA pathfinders
using optical coadding of HI
if you gave them to me
TODAY.
WiggleZ and zCOSMOSWiggleZ zCOSMOS
Instrument/Telescope AAOmega on the AAT VIMOS on the VLT
Target Selectionultraviolet using the
GALEX satelliteoptical I band
IAB < 22.5
Survey Area1000 deg2 total
7 fields minimum size of ~100 deg2
COSMOS fieldsingle field
~2 deg2
Primary Redshift Range
0.5 < z < 1.0 0.1 < z < 1.2
Survey Timeline 2006 to 2010 2005 to 2008
nz by survey end 176,000 20,000
nz in March 2008 ~62,000 ~10,000
WiggleZ and zCOSMOSWiggleZ zCOSMOS
Instrument/Telescope AAOmega on the AAT VIMOS on the VLT
Target Selectionultraviolet using the
GALEX satelliteoptical I band
IAB < 22.5
Survey Area1000 deg2 total
7 fields minimum size of ~100 deg2
COSMOS fieldsingle field
~2 deg2
Primary Redshift Range
0.5 < z < 1.0 0.1 < z < 1.2
Survey Timeline 2006 to 2010 2005 to 2008
nz by survey end 176,000 20,000
nz in March 2008 ~62,000 ~10,000
WiggleZ and zCOSMOSWiggleZ zCOSMOS
Instrument/Telescope AAOmega on the AAT VIMOS on the VLT
Target Selectionultraviolet using the
GALEX satelliteoptical I band
IAB < 22.5
Survey Area1000 deg2 total
7 fields minimum size of ~100 deg2
COSMOS fieldsingle field
~2 deg2
Primary Redshift Range
0.5 < z < 1.0 0.1 < z < 1.2
Survey Timeline 2006 to 2010 2005 to 2008
nz by survey end 176,000 20,000
nz in March 2008 ~62,000 ~10,000
WiggleZ and
ASKAP
WiggleZ field
data as of March 2008 z = 0.1 to 1.0
ASKAP beam size
Diameter 6.2 degreesArea 30 deg2
~10 degrees across
ASKAP & WiggleZ 100hrs
nz = 5975
ASKAP & WiggleZ 100hrs
nz = 5975
ASKAP & WiggleZ 100hrs
nz = 5975
ASKAP & WiggleZ 1000hrs
nz = 5975
zCOSMOS and
MeerKAT
zCOSMOS field
data as of March 2008 z = 0.1 to 1.0
MeerKAT beam size at
1420 MHz z = 0
MeerKAT beam size at
1000 MHz z = 0.4
~1.3 degrees across
MeerKAT & zCOSMOS 100hrs
nz = 7615
MeerKAT & zCOSMOS 100hrs
nz = 7615
MeerKAT & zCOSMOS 100hrs
nz = 7615
MeerKAT & zCOSMOS 1000hrs
nz = 7615
Conclusion
• can use coadding with optical redshifts to make measurement of the HI
21 cm emission from galaxies at redshifts z > 0.1
• the measured cosmic neutral gas density at z = 0.24 is consistent with
that from damped Lyα
• galaxy cluster Abell 370 at z = 0.37 has significantly more gas than
similar clusters at z ~ 0, possibly as much as 10 times more gas
• the SKA pathfinders ASKAP and MeerKAT can measure significant
amounts of HI 21 cm emission out to z = 1.0 using the coadding
technique with existing redshift surveys
Conclusion