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