The Cosmic Evolution of Neutral Atomic Hydrogen Gas Philip Lah Macquarie University Colloquium 27th March 2015
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
How to measure? 1. 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
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 M HI 236 1 z S mjy d L Mpc 2 V kms 1 M HI* = 6.2 10 9 M (Zwaan et al. 2003)
HI 21-cm Emission: The Observations
HI density HIPASS Zwaan05
HI density HIPASS Zwaan05 blind HI 21 cm emission direct detection Zwaan 2005 HIPASS 4315 galaxies
HI density ALFALFA Martin10
HI density ALFALFA Martin10 blind HI 21 cm emission direct detection Martin 2010 ALFALFA 10,119 galaxies
How to measure? 2. Damped Lyman-α Absorption Systems
How to measure? 2. Damped Lyman-α Absorption Systems
Intensity Lyman-α Absorption Systems hydrogen gas clouds observer quasar Lyman-α absorption by clouds Lyman-α emission Wavelength
Intensity Damped Lyman-α QSO 1425+6039 redshift z = 3.2 Keck HIRES optical spectrum Lyα emission Lyman-α forest DLA 4200 4400 4600 4800 5000 5200 Wavelength (Å) Lyman-α 1216 Å rest frame
Damped Lyman-α: The Observations
HI density Noterdaeme09
HI density Noterdaeme09 Damped Lyman-α Noterdaeme 2009 SDSS 937 absorbers
HI density Noterdaeme12
HI density Noterdaeme12 Damped Lyman-α Noterdaeme 2012 BOSS 6839 absorbers
HI density Zafar13
HI density Zafar13 Damped Lyman-α Zafar 2013 UVES 122 quasars
Lower Redshift Damped Lyman-α
HI density Rao06
HI density Rao06 Damped Lyman-α Rao 2006 MgII FeII systems UV HST 197 systems
Coadding HI 21 cm Emission Signals
Coadding HI signals Radio Data Cube DEC RA
Coadding HI signals Radio Data Cube DEC positions of optical galaxies RA
flux Coadding HI signals frequency
flux z1 Coadding HI signals z2 z3 z1, z2 & z3 optical redshifts of galaxies frequency
flux Coadding HI signals z1 z2 Coadded HI signal z3 velocity velocity
flux Coadding HI signals z1 z2 Coadded HI signal z3 velocity velocity Noise m N N = number of galaxies
Coadding HI 21 cm Emission: The Observations
HI density Lah07
HI density Lah07 HI 21 cm emission stacking Lah 2007 GMRT/Subaru/AAT 154 galaxies
HI density Freudling11
HI density Freudling11 HI 21 cm emission targeted Freudling 2011 AUDS Arecibo 18 galaxies
HI density Rhee13
HI density Rhee13 HI 21 cm emission stacking Rhee 2013 WSRT CNOC 59 + 69 galaxies
HI density Delhaize13
HI density Delhaize13 HI 21 cm emission stacking Delhaize 2013 Parkes 2dFGRS 3277 galaxies HIPASS 2dFGRS 15093 galaxies
HI density VVDS14
HI density VVDS14 HI 21 cm emission stacking Rhee thesis VVDS14 GMRT/AAT/MMT 165 galaxies
HI density zcosmos14
HI density zcosmos14 HI 21 cm emission stacking Rhee thesis GMRT/zCOSMOS
HI density Hoppmann14
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 4σ
HI density High z average 7σ
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) Gavazzi et al. 2006 Def HI = 1 is 10% of expected HI gas expected gas estimate based on optical diameter and Hubble type
Cluster Stacking Observations
Abell 370, a galaxy cluster at z = 0.37 large galaxy cluster of order same size as Coma similar cluster velocity dispersion and X-ray gas temperature Abell 370 cluster core, ESO VLT image
Distribution of galaxies around Abell 370 cluster redshifts AAT complete GMRT redshift range
Distribution of galaxies around Abell 370 8 Mpc radius region: 220 galaxies cluster redshift
HI density Outer Cluster Region Inner Cluster Region
HI density Outer Cluster Region Inner Cluster Region
Distribution of galaxies around Abell 370 cluster redshift
Distribution of galaxies around Abell 370 110 galaxies cluster redshift within R 200 region
HI density Outer Cluster Region Inner Cluster Region
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 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
Galaxy Cluster Abell 370
HI Mass vs Star Formation Rate in Abell 370 all 168 [OII] emission galaxies Average line from Doyle & Drinkwater 2006
HI Mass vs Star Formation Rate in Abell 370 Average 81 blue [OII] emission galaxies 87 red [OII] emission galaxies line from Doyle & Drinkwater 2006
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 Average all 168 [OII] emission galaxies line from Bell 2003
Radio Continuum vs. [OII] Star Formation Rate 87 red [OII] emission galaxies Average line from Bell 2003 81 blue [OII] emission galaxies
The Next Generation of Observations
Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12
Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12
Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12
Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12
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 0.26-75% of the entire sky- 9600 hrs DINGO (Deep Investigations of Neutral Gas Origins) - z = 0 to 0.4 - GAMA regions - 7500 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 0.26-75% of the entire sky- 9600 hrs DINGO (Deep Investigations of Neutral Gas Origins) - z = 0 to 0.4 - GAMA regions - 7500 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 0.26-75% of the entire sky- 9600 hrs DINGO (Deep Investigations of Neutral Gas Origins) - z = 0 to 0.4 - GAMA regions - 7500 hrs, ~290 deg 2 FLASH (The First Large Absorption Survey in HI) - a blind HI absorption-line survey, 0.5 < z <1.0, 25000 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
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 small galaxy optical spectrum z = 0.374 within cluster
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 10 57 atoms of hydrogen atoms total HI gas in galaxies ~ 10 7 to 10 10 M HI 21 cm luminosity of ~2 10 32 to 2 10 35 ergs s -1 in star forming galaxies luminosity of H emission ~3 10 39 to 3 10 42 ergs s -1
HI density Molonglo?? Molonglo Bandwidth 3 MHz Centre frequency 843 MHz z = 0.681 to 0.687