The Cosmic Evolution of Neutral Atomic Hydrogen Gas Philip Lah

Transcription

1 The Cosmic Evolution of Neutral Atomic Hydrogen Gas Philip Lah University of Sydney Colloquium 27 November 2014

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

3 Neutral Atomic Hydrogen Gas in Galaxies

4 Galaxy M33: optical

5 Galaxy M33: HI 21-cm emission

6 Galaxy M33: optical and HI

7 Galaxy M33: optical

8 Why Study Neutral Atomic Hydrogen Gas?

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 Why Study Neutral Atomic Hydrogen Gas? Because you can measure it!

13 Why Study Neutral Atomic Hydrogen Gas? Because you can measure it!

14 The Cosmic Evolution of HI Gas

15 Reionisation

16 HI density nothing

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

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

19 Neutral atomic hydrogen creates 21 cm radiation proton electron

20 Neutral atomic hydrogen creates 21 cm radiation

21 Neutral atomic hydrogen creates 21 cm radiation

22 Neutral atomic hydrogen creates 21 cm radiation

23 Neutral atomic hydrogen creates 21 cm radiation photon

24 Neutral atomic hydrogen creates 21 cm radiation

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

26 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)

27 HI 21-cm Emission: The Observations

28 HI density HIPASS Zwaan05

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

30 HI density ALFALFA Martin10

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

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

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

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

35 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

36 Damped Lyman-α: The Observations

37 HI density Noterdaeme09

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

39 HI density Noterdaeme12

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

41 HI density Zafar13

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

43 Lower Redshift Damped Lyman-α

44 HI density Rao06

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

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 Neutral Atomic Hydrogen Gas In Different Environments

72 Nearby Galaxy Clusters Are Deficient In HI Gas

73 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

74 Cluster Stacking Observations

75 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

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

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

78 HI density Outer Cluster Region Inner Cluster Region

79 HI density Outer Cluster Region Inner Cluster Region

80 Distribution of galaxies around Abell 370 cluster redshift

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

82 HI density Outer Cluster Region Inner Cluster Region

83 The Next Generation of Observations

84 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

85 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

86 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

87 Radio Telescopes SKA1 SYSTEM BASELINE DESIGN

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

89 HI density GMRT 1000 MHz ~610 MHz

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

91 HI density JVLA 1000 MHz

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

93 ASKAP 12 m diameter dishes 36 dishes focal plane array

94 HI density ASKAP 700 MHz

95 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

96 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

97 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, 3200 hrs, deeper pointings HI stacking using WiggleZ redshifts

98 MeerKAT South African SKA pathfinder 13.5 m diameter dishes 64 dishes

99 HI density MeerKAT 580 MHz

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

101 The SKA-mid

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

103 HI density SKA-mid 350 MHz

104 Then On To The SKA

105

106 Additional Slides

107 A Radio Gravitational Arc?

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

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

110 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)

111 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.

112 VLA C-band 4860 MHz 30 arcsec on a side Peak 160 µjy/beam

113 VLA L-band 1400 MHz 30 arcsec on a side Peak 350 µjy/beam

114 GMRT 1040 MHz 30 arcsec on a side Peak 490 µjy/beam

115 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

116 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.

117

118 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

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

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

121 Giant Metrewave Radio Telescope