The Cosmic Evolution of Neutral Atomic Hydrogen Gas AAO Colloquium 5th February 2015 Philip Lah

Collaborators: Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (ANU) Roberto De Propris (FINCA) Michael Pracy (USyd) Jonghwan Rhee (UWA)

Why Study Neutral Atomic Hydrogen Gas?

Galaxy M33: optical

Galaxy M33: HI 21-cm emission

Galaxy M33: optical and HI

Galaxy M33: optical

HI Gas and Star Formation neutral atomic hydrogen gas cloud (HI) molecular gas cloud (H 2 ) star formation

The Cosmic Evolution of Star Formation

The History of Star Formation in the Universe

The Cosmic Evolution of HI Gas

HI density – nothing

How to measure? 1. HI 21-cm Emission

Neutral atomic hydrogen creates 21 cm radiation proton electron

Neutral atomic hydrogen creates 21 cm radiation

photon

Neutral atomic hydrogen creates 21 cm radiation

HI 21 cm emission decay half life ~10 million years

HI Mass Assuming an optically thin neutral hydrogen cloud M HI * = 6.2 ×10 9 M  (Zwaan et al. 2003)

HI 21-cm Emission: The Observations

HI density – HIPASS Zwaan05

Zwaan 2005 HIPASS 4315 galaxies blind HI 21 cm emission direct detection

HI density – ALFALFA Martin10

Martin 2010 ALFALFA 10,119 galaxies blind HI 21 cm emission direct detection

How to measure? 2. Damped Lyman-α Absorption Systems

Lyman-α Absorption Systems quasar hydrogen gas clouds Lyman-α emission Lyman-α absorption by clouds Wavelength observer Intensity

Damped Lyman-α Lyman-α 1216 Å rest frame Intensity Wavelength (Å) Lyα emission QSO redshift z = 3.2 Keck HIRES optical spectrum DLA Lyman-α forest

Damped Lyman-α: The Observations

HI density – Noterdaeme09

Noterdaeme 2009 SDSS 937 absorbers Damped Lyman-α

HI density – Noterdaeme12

Noterdaeme 2012 BOSS 6839 absorbers Damped Lyman-α

HI density – Zafar13

Zafar 2013 UVES 122 quasars Damped Lyman-α

Lower Redshift Damped Lyman-α

HI density – Rao06

Rao 2006 MgII–FeII systems UV HST 197 systems Damped Lyman-α

Coadding HI 21 cm Emission Signals

Coadding HI signals RA DEC Radio Data Cube Frequency HI redshift

Coadding HI signals RA DEC Radio Data Cube Frequency HI redshift positions of optical galaxies

Coadding HI signals frequency flux

Coadding HI signals frequency flux z2 z1 z3 z1, z2 & z3 optical redshifts of galaxies

Coadding HI signals velocity z1 z2 z3 flux velocity Coadded HI signal

Coadding HI signals velocity z1 z2 z3 flux velocity Coadded HI signal Noise m√ N N = number of galaxies

Coadding HI 21 cm Emission: The Observations

HI density – Lah07

Lah 2007 GMRT/Subaru/AAT 154 galaxies HI 21 cm emission stacking

HI density – Freudling11

Freudling 2011 AUDS Arecibo 18 galaxies HI 21 cm emission targeted

HI density – Rhee13

Rhee 2013 WSRT CNOC galaxies HI 21 cm emission stacking

HI density – Delhaize13

Delhaize 2013 Parkes 2dFGRS 3277 galaxies HIPASS 2dFGRS galaxies HI 21 cm emission stacking

HI density – VVDS14

HI 21 cm emission stacking Rhee thesis VVDS14 GMRT/AAT/MMT 165 galaxies

HI density – zCOSMOS14

HI 21 cm emission stacking Rhee thesis GMRT/zCOSMOS

HI density – Hoppmann14

HI 21 cm emission targeted Hoppmann 2014 AUDS Arecibo 105 galaxies

HI density – Current Status Current Status

HI density – Low z average 4σ4σ

HI density – High z average 7σ7σ

Neutral Atomic Hydrogen Gas In Different Environments

Nearby Galaxy Clusters Are Deficient In HI Gas

HI Deficiency in Clusters Def HI = log(M HI exp. / M HI obs) Def HI = 1 is 10% of expected HI gas Gavazzi et al expected gas estimate based on optical diameter and Hubble type

Cluster Stacking Observations

Abell 370, a galaxy cluster at z = 0.37 Abell 370 cluster core, ESO VLT image large galaxy cluster of order same size as Coma  similar cluster velocity dispersion and X-ray gas temperature

cluster redshifts AAT Distribution of galaxies around Abell 370 complete GMRT redshift range

Distribution of galaxies around Abell 370 cluster redshift 8 Mpc radius region: 220 galaxies

Inner Cluster Region Outer Cluster Region HI density

Inner Cluster Region Outer Cluster Region HI density

cluster redshift Distribution of galaxies around Abell 370

cluster redshift Distribution of galaxies around Abell 370 within R 200 region 110 galaxies

Inner Cluster Region Outer Cluster Region HI density

Galaxy HI mass vs Star Formation Rate

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

Star Formation In The Fujita Galaxies

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 bright L(Hα) galaxies 42 medium L(Hα) galaxies 37 faint L(Hα) galaxies

Galaxy Cluster Abell 370

HI Mass vs Star Formation Rate in Abell 370 all 168 [OII] emission galaxies line from Doyle & Drinkwater 2006 Average

HI Mass vs Star Formation Rate in Abell blue [OII] emission galaxies line from Doyle & Drinkwater red [OII] emission galaxies Average

Radio Continuum In The Fujita Galaxies

Star Formation Rate from Hα Emission and Radio Continuum Emission

Halpha vs. RC line from Sullivan et al. 2001

Radio Continuum In The Galaxy Cluster Abell 370

Star Formation Rate from [OII] Emission and Radio Continuum Emission

Radio Continuum vs. [OII] Star Formation Rate all 168 [OII] emission galaxies line from Bell 2003 Average

Radio Continuum vs. [OII] Star Formation Rate line from Bell blue [OII] emission galaxies 87 red [OII] emission galaxies Average

The Next Generation of Observations

Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

Giant Metrewave Radio Telescope 45 m diameter dishes 30 dishes low frequency

HI density – GMRT 1000 MHz ~610 MHz

Karl G. Jansky Very Large Array 25 m diameter dishes 27 dishes high frequency

HI density –JVLA 1000 MHz

JVLA HI Survey CHILES (the COSMOS HI Large Extragalactic Survey) – z = 0 to 0.45, 1000 hours in B array

ASKAP 12 m diameter dishes 36 dishes focal plane array

HI density – ASKAP 700 MHz

ASKAP HI Surveys WALLABY (Widefield ASKAP L-Band Legacy All-Sky Blind Survey) - z = 0 to % of the entire sky hrs DINGO (Deep Investigations of Neutral Gas Origins) - z = 0 to GAMA regions hrs, ~290 deg 2 FLASH (The First Large Absorption Survey in HI) - a blind HI absorption-line survey, out to z = 1.0, 3000 deg 2, 2400 hrs, HI stacking using WiggleZ redshifts

ASKAP HI Surveys WALLABY (Widefield ASKAP L-Band Legacy All-Sky Blind Survey) - z = 0 to % of the entire sky hrs DINGO (Deep Investigations of Neutral Gas Origins) - z = 0 to GAMA regions hrs, ~290 deg 2 FLASH (The First Large Absorption Survey in HI) - a blind HI absorption-line survey, out to z = 1.0, 3000 deg 2, 2400 hrs, HI stacking using WiggleZ redshifts

ASKAP HI Surveys WALLABY (Widefield ASKAP L-Band Legacy All-Sky Blind Survey) - z = 0 to % of the entire sky hrs DINGO (Deep Investigations of Neutral Gas Origins) - z = 0 to GAMA regions hrs, ~290 deg 2 FLASH (The First Large Absorption Survey in HI) - a blind HI absorption-line survey, 0.5 < z <1.0, deg 2, 1600 hrs

MeerKAT South African SKA pathfinder 13.5 m diameter dishes 64 dishes

HI density – MeerKAT 580 MHz

MeerKAT HI Surveys LADUMA – (Looking At the Distant Universe with the MeerKAT Array) – going out to z > 1.0, ~5000 hours, single pointing targeting Extended Chandra Deep Field South (ECDF-S)

The SKA-mid

64 × 13.5-m diameter dishes from the MeerKAT array and 190 × 15-m dishes ~15% of full SKA

HI density – SKA-mid 350 MHz

Then On To The SKA

Additional Slides

An Unusual Object In Galaxy Cluster Abell 370

Radio Arc V band optical image from ANU 40 inch Abell 370 cluster 8 arcmin square

Radio Arc V band optical image from ANU 40 inch Abell 370 cluster 8 arcmin square

Radio Arc optical image from Hubble Space Telescope optical arc in Abell 370 was the first detected gravitational lensing event by a galaxy cluster (Soucail et al. 1987)

Radio Arc 50 arcsec on a side radio contour levels start at 28.5 μJy/ beam (3σ) VLA L-band radio data has a synthesised beam size of ∼ 1.5 arcsec.

Radio Arc small galaxy observed with LRIS on Keck optical spectrum z = within cluster s mall galaxy

VLA C-band 4860 MHz 30 arcsec on a side Peak 160 µJy/Beam

VLA L-band 1400 MHz 30 arcsec on a side Peak 350 µJy/Beam

GMRT 1040 MHz 30 arcsec on a side Peak 490 µJy/Beam

Theoretical Model of Arc - based on Parametric Mass Model of Abell 370 by Richard et al. (2010) - images are 30.3 arcsec across, contour spacing geometric progression, with a factor 1.5 in between each contour

HI 21cm emission HI 21 cm emission decay half life ~10 million years 1 M   1.2  atoms of hydrogen atoms total HI gas in galaxies ~ 10 7 to M  HI 21 cm luminosity of ~2  to 2  ergs s -1 in star forming galaxies  luminosity of H  emission ~3  to 3  ergs s -1

HI density –Molonglo?? Molonglo Bandwidth 3 MHz Centre frequency 843 MHz z = to 0.687