The Cosmic Evolution of Neutral Atomic Hydrogen Gas. Philip Lah. Macquarie University Colloquium 27th March 2015

Transcription

1 The Cosmic Evolution of Neutral Atomic Hydrogen Gas Philip Lah Macquarie University Colloquium 27th March 2015

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

3

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

12

13 The Cosmic Evolution of HI Gas

14 HI density nothing

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

16 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

19 Neutral atomic hydrogen creates 21 cm radiation

20 Neutral atomic hydrogen creates 21 cm radiation

21 Neutral atomic hydrogen creates 21 cm radiation photon

22 Neutral atomic hydrogen creates 21 cm radiation

23 Neutral atomic hydrogen creates 21 cm radiation HI 21 cm emission decay half life ~10 million years

24 HI Mass Assuming an optically thin neutral hydrogen cloud M M HI z S mjy d L Mpc 2 V kms 1 M HI* = M (Zwaan et al. 2003)

25 HI 21-cm Emission: The Observations

26 HI density HIPASS Zwaan05

27 HI density HIPASS Zwaan05 blind HI 21 cm emission direct detection Zwaan 2005 HIPASS 4315 galaxies

28 HI density ALFALFA Martin10

29 HI density ALFALFA Martin10 blind HI 21 cm emission direct detection Martin 2010 ALFALFA 10,119 galaxies

30

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

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

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

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

35 Damped Lyman-α: The Observations

36 HI density Noterdaeme09

37 HI density Noterdaeme09 Damped Lyman-α Noterdaeme 2009 SDSS 937 absorbers

38 HI density Noterdaeme12

39 HI density Noterdaeme12 Damped Lyman-α Noterdaeme 2012 BOSS 6839 absorbers

40 HI density Zafar13

41 HI density Zafar13 Damped Lyman-α Zafar 2013 UVES 122 quasars

42 Lower Redshift Damped Lyman-α

43 HI density Rao06

44 HI density Rao06 Damped Lyman-α Rao 2006 MgII FeII systems UV HST 197 systems

45

46 Coadding HI 21 cm Emission Signals

47 Coadding HI signals Radio Data Cube DEC RA

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

49 flux Coadding HI signals frequency

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

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

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

53 Coadding HI 21 cm Emission: The Observations

54 HI density Lah07

55 HI density Lah07 HI 21 cm emission stacking Lah 2007 GMRT/Subaru/AAT 154 galaxies

56 HI density Freudling11

57 HI density Freudling11 HI 21 cm emission targeted Freudling 2011 AUDS Arecibo 18 galaxies

58 HI density Rhee13

59 HI density Rhee13 HI 21 cm emission stacking Rhee 2013 WSRT CNOC galaxies

60 HI density Delhaize13

61 HI density Delhaize13 HI 21 cm emission stacking Delhaize 2013 Parkes 2dFGRS 3277 galaxies HIPASS 2dFGRS galaxies

62 HI density VVDS14

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

64 HI density zcosmos14

65 HI density zcosmos14 HI 21 cm emission stacking Rhee thesis GMRT/zCOSMOS

66 HI density Hoppmann14

67 HI density Hoppmann14 HI 21 cm emission targeted Hoppmann 2014 AUDS Arecibo 105 galaxies

68 HI density Current Status Current Status

69 HI density Low z average 4σ

70 HI density High z average 7σ

71

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) Gavazzi et al Def HI = 1 is 10% of expected HI gas expected gas estimate based on optical diameter and Hubble type

75 Cluster Stacking Observations

76 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

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

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

79 HI density Outer Cluster Region Inner Cluster Region

80 HI density Outer Cluster Region Inner Cluster Region

81 Distribution of galaxies around Abell 370 cluster redshift

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

83 HI density Outer Cluster Region Inner Cluster Region

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 all 121 galaxies line from Doyle & Drinkwater 2006

88 HI Mass vs Star Formation Rate at z = bright L(Hα) galaxies line from Doyle & Drinkwater 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 Average line from Doyle & Drinkwater 2006

91 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

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 Average all 168 [OII] emission galaxies line from Bell 2003

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

99

100 The Next Generation of Observations

101 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

102 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

103 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

104 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

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 % 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

113 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

114 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

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 The SKA-mid m diameter dishes from the MeerKAT array and m dishes ~15% of full SKA

120 HI density SKA-mid 350 MHz

121 Then On To The SKA

122

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 small galaxy optical spectrum z = within cluster

130

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 atoms of hydrogen atoms total HI gas in galaxies ~ 10 7 to M HI 21 cm luminosity of ~ to ergs s -1 in star forming galaxies luminosity of H emission ~ to ergs s -1

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