HI in Galaxies at Redshifts 0.1 to 1.0: Current and Future Observations Using Optical Redshifts for HI Coadding. Philip Lah

Size: px

Start display at page:

Download "HI in Galaxies at Redshifts 0.1 to 1.0: Current and Future Observations Using Optical Redshifts for HI Coadding. Philip Lah"

Vivian Adams
5 years ago
Views:

1 HI in Galaxies at Redshifts 0.1 to 1.0: Current and Future Observations Using Optical Redshifts for HI Coadding Philip Lah Deep Surveys of the Radio Universe with SKA Pathfinders

2 Collaborators: Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (AAO) Roberto De Propris (CTIO) Michael Pracy (ANU)

3 Current Observations Talk Outline HI in star forming galaxies at z = 0.24 HI in Abell 370, a galaxy cluster at z = 0.37 Future Observations using ASKAP and WiggleZ using MeerKAT and zcosmos

4 Current Observations - HI coadding

5 Giant Metrewave Radio Telescope

6 Giant Metrewave Radio Telescope

7 Anglo-Australian Telescope

8 2dF/AAOmega instrument multi-object, fibre fed spectrograph

9 The Fujita galaxies Hα emission galaxies at z = 0.24

10 The Fujita Galaxies Subaru Field 24! 30 DEC narrow band imaging H" emission at z = 0.24 (Fujita et al. 2003, ApJL, 586, L115) 348 Fujita galaxies 121 redshifts using AAT GMRT ~48 hours on field RA

11 Coadded HI Spectrum

12 Fujita galaxies neutral hydrogen gas measurement raw HI spectrum all using 121 redshifts - weighted average binned M HI = (2.26 ± 0.90)!10 9 M

13 The Cosmic Hydrogen Gas Density

14 my new point The Cosmic Gas Density vs. Redshift

15 my new point Cosmic Neutral Gas Density vs. Time

16 Abell 370 a galaxy cluster at z = 0.37

17 Abell 370 large galaxy cluster at z = 0.37, of order same size of Coma similar cluster velocity dispersion and X-ray gas temperature optical imaging ANU 40 inch telescope spectroscopic follow-up with the AAT GMRT ~34 hours on cluster

18 Abell 370 galaxy cluster Abell 370 galaxy cluster 324 galaxies with redshifts z = to blue galaxies 219 red galaxies

19 Abell 370 galaxy cluster Abell 370 galaxy cluster 3# extent of X-ray gas R 200 radius at which cluster 200 times denser than the general field

20 The Measuring the HI signal

21 Galaxy Sizes For HI stacking I want the galaxies to be unresolved. For the Fujita galaxies I used an estimate of the HI size from the optical properties using information on nearby spiral and irregular field galaxies. Complication! The Abell 370 galaxies are a mixture of early and late types in a variety of environments. Solution I made multiple measurements of the galaxies HI mass using different smoothing sizes.

22 Galaxy Sizes For HI stacking I want the galaxies to be unresolved. For the Fujita galaxies I used an estimate of the HI size from the optical properties using information on nearby spiral and irregular field galaxies. Complication! The Abell 370 galaxies are a mixture of early and late types in a variety of environments. Solution I made multiple measurements of the galaxies HI mass using different smoothing sizes.

23 Galaxy Sizes For HI stacking I want the galaxies to be unresolved. For the Fujita galaxies I used an estimate of the HI size from the optical properties using information on nearby spiral and irregular field galaxies. Complication! The Abell 370 galaxies are a mixture of early and late types in a variety of environments. Solution I made multiple measurements of the galaxies HI mass using different smoothing sizes.

24 The Average HI Mass Measurements

25 HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

26 HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

27 HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

28 HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

29 HI mass 324 galaxies 219 galaxies 105 galaxies 94 galaxies 156 galaxies 168 galaxies 104 galaxies 220 galaxies

30 HI spectra Large Smoothing M HI = (6.6 ± 3.5)!10 9 M M HI = (23.0 ± 7.7)!10 9 M

31 HI Flux All Galaxies 30 arcsec across ~150 kpc across

32 HI Flux The Blue Galaxies Outside X-ray Gas 30 arcsec across ~150 kpc across

33 Future Observations - HI coadding

34 What I could do with the SKA pathfinders if you gave them to me TODAY.

35 ASKAP and MeerKAT ASKAP parameters MeerKAT Number of Dishes Dish Diameter 12 m 12 m Aperture Efficiency System Temp. 35 K 30 K Frequency range MHz MHz Instantaneous bandwidth 300 MHz 512 MHz Field of View: at 1420 MHz (z = 0) at 700 MHz (z = 1) 30 deg 2 30 deg deg deg 2 Maximum Baseline Length 8 km 10 km

36 ASKAP and MeerKAT ASKAP parameters MeerKAT Number of Dishes Dish Diameter 12 m 12 m Aperture Efficiency System Temp. 35 K 30 K Frequency range MHz MHz Instantaneous bandwidth 300 MHz 512 MHz Field of View: at 1420 MHz (z = 0) at 700 MHz (z = 1) 30 deg 2 30 deg deg deg 2 Maximum Baseline Length 8 km 10 km

37 ASKAP and MeerKAT ASKAP parameters MeerKAT Number of Dishes Dish Diameter 12 m 12 m Aperture Efficiency System Temp. 35 K 30 K Frequency range MHz MHz Instantaneous bandwidth 300 MHz 512 MHz Field of View: at 1420 MHz (z = 0) at 700 MHz (z = 1) z = 0.4 to 1.0 in a single 30 observation deg 2 30 deg 2 z = 0.2 to 1.0 in a single 1.2 observation deg deg 2 Maximum Baseline Length 8 km 10 km

38 WiggleZ and WiggleZ zcosmos zcosmos Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection Survey Area ultraviolet using the GALEX satellite 1000 deg 2 total 7 fields minimum size of ~100 deg 2 optical I band I AB < 22.5 COSMOS field single field ~2 deg 2 Primary Redshift Range 0.5 < z < < z < 1.2 Survey Timeline 2006 to to 2008 n z by survey end 176,000 20,000 n z in March 2008 ~62,000 ~10,000

39 WiggleZ and WiggleZ zcosmos zcosmos Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection Survey Area ultraviolet using the GALEX satellite 1000 deg 2 total 7 fields minimum size of ~100 deg 2 optical I band I AB < 22.5 COSMOS field single field ~2 deg 2 Primary Redshift Range 0.5 < z < < z < 1.2 Survey Timeline 2006 to to 2008 n z by survey end 176,000 20,000 n z in March 2008 ~62,000 ~10,000

40 WiggleZ and WiggleZ zcosmos zcosmos Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection Survey Area ultraviolet using the GALEX satellite 1000 deg 2 total 7 fields minimum size of ~100 deg 2 optical I band I AB < 22.5 COSMOS field single field ~2 deg 2 Primary Redshift Range 0.5 < z < < z < 1.2 Survey Timeline 2006 to to 2008 n z by survey end 176,000 20,000 n z in March 2008 ~62,000 ~10,000

41 WiggleZ and WiggleZ zcosmos zcosmos Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection Survey Area ultraviolet using the GALEX satellite 1000 deg 2 total 7 fields minimum size of ~100 deg 2 optical I band I AB < 22.5 COSMOS field single field ~2 deg 2 Primary Redshift Range 0.5 < z < < z < 1.2 Survey Timeline 2006 to to 2008 n z by survey end 176,000 20,000 n z in March 2008 ~62,000 ~10,000

42 WiggleZ and WiggleZ zcosmos zcosmos Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection Survey Area ultraviolet using the GALEX satellite 1000 deg 2 total 7 fields minimum size of ~100 deg 2 optical I band I AB < 22.5 COSMOS field single field ~2 deg 2 Primary Redshift Range 0.5 < z < < z < 1.2 Survey Timeline 2006 to to 2008 n z by survey end 176,000 20,000 n z in March 2008 ~62,000 ~10,000

43 WiggleZ and WiggleZ zcosmos zcosmos Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection Survey Area ultraviolet using the GALEX satellite 1000 deg 2 total 7 fields minimum size of ~100 deg 2 optical I band I AB < 22.5 COSMOS field single field ~2 deg 2 Primary Redshift Range 0.5 < z < < z < 1.2 Survey Timeline 2006 to to 2008 n z by survey end 176,000 20,000 n z in March 2008 ~62,000 ~10,000

44 WiggleZ and WiggleZ zcosmos zcosmos Instrument/Telescope AAOmega on the AAT VIMOS on the VLT Target Selection Survey Area ultraviolet using the GALEX satellite 1000 deg 2 total 7 fields minimum size of ~100 deg 2 optical I band I AB < 22.5 COSMOS field single field ~2 deg 2 Primary Redshift Range 0.5 < z < < z < 1.2 Survey Timeline 2006 to to 2008 n z by survey end 176,000 20,000 n z in March 2008 ~62,000 ~10,000

45 WiggleZ and ASKAP

46 WiggleZ field ~10 degrees across data as of March 2008 z = 0.1 to 1.0 ASKAP beam size Diameter 6.2 degrees Area 30 deg 2

47 ASKAP & WiggleZ 100hrs n z = 5975

48 ASKAP & WiggleZ 100hrs n z = 5975

49 ASKAP & WiggleZ 100hrs n z = 5975

50 ASKAP & WiggleZ 1000hrs n z = 5975

51 zcosmos and MeerKAT

52 zcosmos field MeerKAT beam size at 1420 MHz z = 0 MeerKAT beam size at 1000 MHz z = 0.4 ~1.3 degrees across data as of March 2008 z = 0.1 to 1.0

53 MeerKAT & zcosmos 100hrs n z = 7615

54 MeerKAT & zcosmos 100hrs n z = 7615

55 MeerKAT & zcosmos 100hrs n z = 7615

56 MeerKAT & zcosmos 1000hrs n z = 7615

57 Conclusion

58 Conclusion can use coadding with optical redshifts to make measurement of the HI 21 cm emission from galaxies at redshifts z > 0.1 the measured cosmic neutral gas density at z = 0.24 is consistent with that from damped Ly" measurements galaxy cluster Abell 370 at z = 0.37 has significantly amounts of neutral hydrogen gas the SKA pathfinders ASKAP and MeerKAT can measure significant amounts of HI 21 cm emission out to z = 1.0 using the coadding technique with existing optical redshift surveys

Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24 Philip Lah. HI Survival Through Cosmic Times Conference

Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24 Philip Lah HI Survival Through Cosmic Times Conference Collaborators: Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (AAO) Roberto De