HI in Galaxies at Redshifts 0 1 to

HI in Galaxies at Redshifts 0. 1 to 1. 0: Current and Future Observations Using Optical Redshifts for HI Coadding Philip Lah Melbourne 2008

Collaborators: Michael Pracy (ANU) Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (AAO) Roberto De Propris (CTIO)

Talk Outline Introduction • Evolution in clusters & star formation rate density vs z • HI 21 cm 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 Wiggle. Z • using Meer. KAT and z. COSMOS

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 Gas Density

The Cosmic Gas Density vs. Redshift Prochaska et al. 2005 DLAs Zwaan et al. 2005 HIPASS HI 21 cm Rao et al. 2006 DLAs from Mg. II absorption

The Cosmic Gas Density vs. Redshift Prochaska et al. 2005 DLAs Zwaan et al. 2005 HIPASS HI 21 cm Rao et al. 2006 DLAs from Mg. II absorption

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 21 cm emission HI 21 cm emission decay half life ~10 million years (3 1014 s) • 1 M 2. 0 1033 g 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 21 cm emission HI 21 cm emission decay half life ~10 million years (3 1014 s) • 1 M 2. 0 1033 g 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 21 cm emission HI 21 cm emission decay half life ~10 million years (3 1014 s) • 1 M 2. 0 1033 g 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 21 cm emission HI 21 cm emission decay half life ~10 million years (3 1014 s) • 1 M 2. 0 1033 g 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 21 cm emission HI 21 cm emission decay half life ~10 million years (3 1014 s) • 1 M 2. 0 1033 g 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 21 cm emission HI 21 cm emission decay half life ~10 million years (3 1014 s) • 1 M 2. 0 1033 g 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 21 cm emission HI 21 cm emission decay half life ~10 million years (3 1014 s) • 1 M 2. 0 1033 g 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 21 cm Emission at High Redshift

HI 21 cm 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 5 109 to 4 1010 M (Verheijen et al. 2007, Ap. JL, 668, L 9) • 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 21 cm 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 5 109 to 4 1010 M (Verheijen et al. 2007, Ap. JL, 668, L 9) • 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 21 cm 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 5 109 to 4 1010 M (Verheijen et al. 2007, Ap. JL, 668, L 9) • 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 21 cm 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 5 109 to 4 1010 M (Verheijen et al. 2007, Ap. JL, 668, L 9) • 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 Radio Data Cube y c n e u ft q i e h s Fr d e r I H DEC RA

Coadding HI signals Radio Data Cube y c n e u ft q i e h s Fr d e r I H DEC positions of optical galaxies RA

flux Coadding HI signals frequency

z 1 Coadding HI signals flux z 2 z 3 frequency

z 1 Coadding HI signals HI signal flux z 2 z 3 frequency velocity

Current Observations HI coadding

Giant Metrewave Radio Telescope

Giant Metrewave Radio Telescope

Giant Metrewave Radio Telescope

Anglo-Australian Telescope

2 d. F/AAOmega instrument multi-object, fibre fed spectrograph

The Fujita galaxies H emission galaxies at z = 0. 24

The Subaru Telescope

The Surprime-cam filters H at z = 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, Ap. JL, 586, L 115) DEC 348 Fujita galaxies 121 redshifts using AAT GMRT ~48 hours on field RA

SFRD vs z - Fujita et al. 2003 Hopkins 2004

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

Fujita galaxies neutral hydrogen gas measurement raw HI spectrum allusing 121 redshifts weighted average binned MHI = (2. 26 ± 0. 90) × 109 M

The Cosmic Neutral Gas Density

The Cosmic Gas Density vs. Redshift my new point

Cosmic Neutral Gas Density vs. Time my new point

Galaxy HI mass vs Star Formation Rate

Galaxy HI Mass vs Star Formation Rate HIPASS & IRAS data z~0 Doyle & Drinkwater 2006

HI Mass vs Star Formation Rate at z = 0. 24 all 121 galaxies line from Doyle & Drinkwater 2006

HI Mass vs Star Formation Rate at z = 0. 24 42 bright L(Hα) galaxies line from Doyle & Drinkwater 2006 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 followup with the AAT GMRT ~34 hours on cluster

Abell 370 – R band images Thumbnails 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 (BV > 0. 57)

Abell 370 galaxy cluster 3σ extent of X-ray gas R 200 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 mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

HI all spectrum all 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 gas blue 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 104 galaxies 324 galaxies 220 galaxies

Abell 370 and Coma Comparison 104 galaxies 324 galaxies 220 galaxies

Abell 370 and Coma Comparison 104 galaxies 324 galaxies 220 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 & IRAS data z~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 92 red [OII] emission galaxies line from Doyle & Drinkwater 2006

Future Observations HI coadding

ASKAP

Meer. KAT South African SKA pathfinder

ASKAP and Meer. KAT ASKAP parameters Meer. KAT Number of Dishes Dish Diameter Aperture Efficiency System Temp. Frequency range Instantaneous bandwidth Field of View: at 1420 MHz (z = 0) at 700 MHz (z = 1) Maximum Baseline Length 45 80 12 m 0. 8 35 K 30 K 700 – 1800 MHz 700 – 10000 MHz 300 MHz 512 MHz 30 deg 2 1. 2 deg 2 4. 8 deg 2 8 km 10 km

ASKAP and Meer. KAT ASKAP parameters Meer. KAT Number of Dishes Dish Diameter Aperture Efficiency System Temp. Frequency range Instantaneous bandwidth Field of View: at 1420 MHz (z = 0) at 700 MHz (z = 1) Maximum Baseline Length 45 80 12 m 0. 8 35 K 30 K 700 – 1800 MHz 700 – 10000 MHz 300 MHz 512 MHz 30 deg 2 1. 2 deg 2 4. 8 deg 2 8 km 10 km

ASKAP and Meer. KAT ASKAP parameters Meer. KAT Number of Dishes Dish Diameter Aperture Efficiency System Temp. Frequency range Instantaneous bandwidth Field of View: at 1420 MHz (z = 0) at 700 MHz (z = 1) Maximum Baseline Length 45 80 12 m 0. 8 35 K 30 K 700 – 1800 MHz 700 – 10000 MHz 300 MHz 512 MHz z = 0. 4 to 1. 0 in a single 30 observation deg 2 z = 0. 2 to 1. 0 in a single 1. 2 observation deg 2 30 deg 2 4. 8 deg 2 8 km 10 km

HI detections ASKAP 100 hr

HI detections ASKAP 1000 hr

HI detections Meer. KAT 100 hr

HI detections Meer. KAT 1000 hr

What I could do with the SKA pathfinders using optical coadding of HI if you gave them to me TODAY.

Wiggle. Z and z. COSMOS Wiggle. Z z. COSMOS Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection ultraviolet using the GALEX satellite optical I band IAB < 22. 5 Survey Area 1000 deg 2 total 7 fields minimum size of ~100 deg 2 COSMOS field single field ~2 deg 2 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

Wiggle. Z and z. COSMOS Wiggle. Z z. COSMOS Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection ultraviolet using the GALEX satellite optical I band IAB < 22. 5 Survey Area 1000 deg 2 total 7 fields minimum size of ~100 deg 2 COSMOS field single field ~2 deg 2 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

Wiggle. Z and z. COSMOS Wiggle. Z z. COSMOS Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection ultraviolet using the GALEX satellite optical I band IAB < 22. 5 Survey Area 1000 deg 2 total 7 fields minimum size of ~100 deg 2 COSMOS field single field ~2 deg 2 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

Wiggle. Z and ASKAP

Wiggle. Z field ~10 degrees across data as of March 2008 z = 0. 1 to 1. 0 ASKAP beam size Diameter 6. 2 degrees Area 30 deg 2

ASKAP & Wiggle. Z 100 hrs nz = 5975

ASKAP & Wiggle. Z 100 hrs nz = 5975

ASKAP & Wiggle. Z 100 hrs nz = 5975

ASKAP & Wiggle. Z 1000 hrs nz = 5975

z. COSMOS and Meer. KAT

z. COSMOS field Meer. KAT beam size at 1420 MHz z = 0 Meer. KAT beam size at 1000 MHz z = 0. 4 ~1. 3 degrees across data as of March 2008 z = 0. 1 to 1. 0

Meer. KAT & z. COSMOS 100 hrs nz = 7615

Meer. KAT & z. COSMOS 100 hrs nz = 7615

Meer. KAT & z. COSMOS 100 hrs nz = 7615

Meer. KAT & z. COSMOS 1000 hrs nz = 7615

Conclusion

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 Meer. KAT can measure significant amounts of HI 21 cm emission out to z = 1. 0 using the coadding technique with existing redshift surveys