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

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

4. Why Study Neutral Atomic Hydrogen Gas?

5. Galaxy M33: optical

6. Galaxy M33: HI 21-cm emission

7. Galaxy M33: optical and HI

8. Galaxy M33: optical

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

10. The Cosmic Evolution of Star Formation

11. The History of Star Formation in the Universe

13. The Cosmic Evolution of HI Gas

14. HI density – nothing

15. How to measure? 1. HI 21-cm Emission

17. Neutral atomic hydrogen creates 21 cm radiation proton electron

18. Neutral atomic hydrogen creates 21 cm radiation

21. photon

22. Neutral atomic hydrogen creates 21 cm radiation

23. HI 21 cm emission decay half life ~10 million years

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

25. HI 21-cm Emission: The Observations

26. HI density – HIPASS Zwaan05

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

28. HI density – ALFALFA Martin10

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

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

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

34. Damped Lyman-α Lyman-α 1216 Å rest frame Intensity Wavelength (Å) 4200440046004800 50005200 Lyα emission QSO 1425+6039 redshift z = 3.2 Keck HIRES optical spectrum DLA Lyman-α forest

35. Damped Lyman-α: The Observations

36. HI density – Noterdaeme09

37. Noterdaeme 2009 SDSS 937 absorbers Damped Lyman-α

38. HI density – Noterdaeme12

39. Noterdaeme 2012 BOSS 6839 absorbers Damped Lyman-α

40. HI density – Zafar13

41. Zafar 2013 UVES 122 quasars Damped Lyman-α

42. Lower Redshift Damped Lyman-α

43. HI density – Rao06

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

46. Coadding HI 21 cm Emission Signals

47. Coadding HI signals RA DEC Radio Data Cube Frequency HI redshift

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

49. Coadding HI signals frequency flux

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

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

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

53. Coadding HI 21 cm Emission: The Observations

54. HI density – Lah07

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

56. HI density – Freudling11

57. Freudling 2011 AUDS Arecibo 18 galaxies HI 21 cm emission targeted

58. HI density – Rhee13

59. Rhee 2013 WSRT CNOC 59 + 69 galaxies HI 21 cm emission stacking

60. HI density – Delhaize13

61. Delhaize 2013 Parkes 2dFGRS 3277 galaxies HIPASS 2dFGRS 15093 galaxies HI 21 cm emission stacking

62. HI density – VVDS14

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

64. HI density – zCOSMOS14

65. HI 21 cm emission stacking Rhee thesis GMRT/zCOSMOS

66. HI density – Hoppmann14

67. HI 21 cm emission targeted Hoppmann 2014 AUDS Arecibo 105 galaxies

68. HI density – Current Status Current Status

69. HI density – Low z average 4σ4σ

70. HI density – High z average 7σ7σ

72. Neutral Atomic Hydrogen Gas In Different Environments

73. Nearby Galaxy Clusters Are Deficient In HI Gas

74. 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. 2006 expected gas estimate based on optical diameter and Hubble type

75. Cluster Stacking Observations

76. 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

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

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

79. Inner Cluster Region Outer Cluster Region HI density

80. Inner Cluster Region Outer Cluster Region HI density

81. cluster redshift Distribution of galaxies around Abell 370

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

83. Inner Cluster Region Outer Cluster Region HI density

84. Galaxy HI mass vs Star Formation Rate

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

86. Star Formation In The Fujita Galaxies

87. HI Mass vs Star Formation Rate at z = 0.24 line from Doyle & Drinkwater 2006 all 121 galaxies

88. 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

89. Galaxy Cluster Abell 370

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

91. HI Mass vs Star Formation Rate in Abell 370 81 blue [OII] emission galaxies line from Doyle & Drinkwater 2006 87 red [OII] emission galaxies Average

92. Radio Continuum In The Fujita Galaxies

93. Star Formation Rate from Hα Emission and Radio Continuum Emission

94. Halpha vs. RC line from Sullivan et al. 2001

95. Radio Continuum In The Galaxy Cluster Abell 370

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

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

98. Radio Continuum vs. [OII] Star Formation Rate line from Bell 2003 81 blue [OII] emission galaxies 87 red [OII] emission galaxies Average

100. The Next Generation of Observations

101. Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12

102. Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12

103. Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12

104. Radio Telescopes SKA1 SYSTEM BASELINE DESIGN 2013-03-12

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

106. HI density – GMRT 1000 MHz ~610 MHz

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

108. HI density –JVLA 1000 MHz

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

110. ASKAP 12 m diameter dishes 36 dishes focal plane array

111. HI density – ASKAP 700 MHz

112. 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

113. 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

114. 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

115. MeerKAT South African SKA pathfinder 13.5 m diameter dishes 64 dishes

116. HI density – MeerKAT 580 MHz

117. 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)

118. The SKA-mid

119. 64 × 13.5-m diameter dishes from the MeerKAT array and 190 × 15-m dishes ~15% of full SKA

120. HI density – SKA-mid 350 MHz

121. Then On To The SKA

123. Additional Slides

124. An Unusual Object In Galaxy Cluster Abell 370

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

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

127. 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)

128. 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.

129. Radio Arc small galaxy observed with LRIS on Keck optical spectrum z = 0.374 within cluster s mall galaxy

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

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

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

134. 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

135. 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

136. HI density –Molonglo?? Molonglo Bandwidth 3 MHz Centre frequency 843 MHz z = 0.681 to 0.687