A pathfinder to the SKA and its pathfinders HILES Team University - - PowerPoint PPT Presentation

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A pathfinder to the SKA and its pathfinders HILES Team University - - PowerPoint PPT Presentation

Sep 01, 2022 352 likes •682 views

Ximena Fernndez Columbia University A pathfinder to the SKA and its pathfinders HILES Team University of Wisconsin West Virginia University Eric Wilcots Columbia University Matthew Bershady D.J. Pisano Charee Peters Lucas Hunt

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SLIDE 1

Ximena Fernández

Columbia University

A pathfinder to the SKA and its pathfinders

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SLIDE 2

HILES Team

Columbia University

Jacqueline van Gorkom Julia Gross David Schiminovich David Hendel Ximena Fernández

West Virginia University

D.J. Pisano Lucas Hunt

University of Wisconsin

Eric Wilcots Matthew Bershady Charee Peters

UMASS- Amherst

Min Yun Hansung Gim

NRAO

Emmanuel Momjian John Hibbard Jennifer Donovan-Meyer

Groningen/ASTRON

Tom Oosterloo Marc Verheijen Rien van de Weygaert

MPIA

Kathryn Kreckel

University of Cape Town

Kelley Hess Danielle Lucero Natasha Maddox Claude Carignan Amidou Sorgho

UWA/ICRAR

Attila Popping Martin Meyer Andreas Wicenec

Michigan State

Laura Chomiuk

University of New Mexico

Patricia Henning Genevieve Vaive

Caltech/JPL

NIck Scoville Joe Lazio

Yonsei University

Aeree Chung

+ CHILES CON POL

(commensal survey led by Chris Hales)

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SLIDE 3

Key questions:

How do galaxies lose their gas? How do galaxies accrete their gas?

Putman et al 2012

What is the relationship between SFR and gas?

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SLIDE 4

Key questions:

How do galaxies lose their gas? How do galaxies accrete their gas?

Putman et al 2012

How does it change as a function of environment and across cosmic time? What is the relationship between SFR and gas?

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SLIDE 5

HI Imaging in the Nearby Universe

NGC 4402 (Chung et al. 2009)

  • Galaxies in clusters: galaxies lose their gas

due to interactions with the ICM

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SLIDE 6

HI Imaging in the Nearby Universe

NGC 4402 (Chung et al. 2009)

  • Galaxies in clusters: galaxies lose their gas

due to interactions with the ICM

KK 246 (Kreckel et al. 2010)

  • Galaxies in voids: evidence for on-going

accretion

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SLIDE 7

Studies of SFR & Gas at z~0

Bigiel et al. 2010

Filled contours: Inside r25

ISM dominated by molecular gas

Empty contours: Outside r25

ISM dominated by HI

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SLIDE 8

Blind HI surveys

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SLIDE 9

WSRT Observations of Abell 963 & 2192 (Verheijen et al. 2007)

1 1

Blind HI surveys

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SLIDE 10

EVLA HI Deep Field Pilot (Fernández et al. 2013)

WSRT Observations of Abell 963 & 2192 (Verheijen et al. 2007)

1 1

Blind HI surveys

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SLIDE 11

VLA HI Deep Field EVLA HI Deep Field Pilot (Fernández et al. 2013)

WSRT Observations of Abell 963 & 2192 (Verheijen et al. 2007)

1 1

Blind HI surveys

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SLIDE 12

VLA HI Deep Field EVLA HI Deep Field Pilot (Fernández et al. 2013)

WSRT Observations of Abell 963 & 2192 (Verheijen et al. 2007)

1 1

Blind HI surveys

+ MeerKat, ASKAP & SKA

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SLIDE 13

An Upgraded VLA

Bandwidth (MHz) 6.25 240 480 Channels 31 16384 30720 Velocity resolution (km/s) 40 3.5 3.5 Instantaneous z coverage 0<z<0.004 0<z<0.193 0<z<0.5 OLD PILOT NOW

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SLIDE 14

CHILES Science Drivers

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SLIDE 15

CHILES Science Drivers

  • 1. HI images in different environments across cosmic time
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SLIDE 16

CHILES Science Drivers

  • 1. HI images in different environments across cosmic time
  • In combination with ALMA, we can study SFR properties in selected systems
  • HI images will provide constraints to simulations to study gas accretion and removal processes.
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SLIDE 17

CHILES Science Drivers

  • 1. HI images in different environments across cosmic time
  • 2. How does the HI mass function (HIMF) evolve with redshift and environment?
  • In combination with ALMA, we can study SFR properties in selected systems
  • HI images will provide constraints to simulations to study gas accretion and removal processes.
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SLIDE 18

CHILES Science Drivers

  • 1. HI images in different environments across cosmic time
  • 2. How does the HI mass function (HIMF) evolve with redshift and environment?
  • In combination with ALMA, we can study SFR properties in selected systems
  • HI images will provide constraints to simulations to study gas accretion and removal processes.
  • Our survey will probe the evolution of the high-mass end of the HIMF
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SLIDE 19

CHILES Science Drivers

  • 1. HI images in different environments across cosmic time
  • 2. How does the HI mass function (HIMF) evolve with redshift and environment?
  • 3. How does the cosmic HI gas density evolve with time?
  • In combination with ALMA, we can study SFR properties in selected systems
  • HI images will provide constraints to simulations to study gas accretion and removal processes.
  • Our survey will probe the evolution of the high-mass end of the HIMF
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SLIDE 20

CHILES Science Drivers

  • 1. HI images in different environments across cosmic time
  • 2. How does the HI mass function (HIMF) evolve with redshift and environment?
  • 3. How does the cosmic HI gas density evolve with time?
  • Our survey will help constrain ΩHI in the interval 0 < z < 0.5
  • In combination with ALMA, we can study SFR properties in selected systems
  • HI images will provide constraints to simulations to study gas accretion and removal processes.
  • Our survey will probe the evolution of the high-mass end of the HIMF
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SLIDE 21
  • Survey led by Chris Hales
  • Full polarization continuum image
  • Noise: 400 nano-Jy/beam
  • Science goals: galaxy evolution, transients,

weak lensing and cosmic magnetism

Commensal Observing

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SLIDE 22

Observation Setup

  • B array observations (5” resolution)
  • Spatial: 0.68-29 kpc
  • 1002 hours of requested time scheduled over 3 B-arrays
  • Observations started Fall 2013
  • Correlator setup:
  • Frequency dithering: 3 frequencies settings (941-1420 MHz)
  • 30,720 channels each of ~3.5 km/s
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SLIDE 23

Target: COSMOS Field

COSMOS: 2 SQ DEGREES CHILES POINTING: ~0.5 DEGREES

  • 1. Deep multiwavelength data
  • 2. No strong radio continuum sources
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SLIDE 24

HI Deep Field

Survey design: detect 3 x 1010 M⦿

1002 hours 60 hours

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SLIDE 25

A Pilot for CHILES: z<0.2

Fernández et al. 2013

33 HI detections in different environments across cosmic time

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SLIDE 26

Full Survey: HI Predictions

~ 300 5σ detections

HIMF Photometric

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SLIDE 27

Full Survey

  • 178/1002 hours done
  • Data reduction is mostly done
  • modified the NRAO pipeline for our observations
  • 1.5 TB per 6 hours, pipeline runs for 60 hours
  • uv gridder: new imaging task developed
  • 2 TB (compared to 100 TB)
  • testing phase
  • Expect to make cube of the first 178 hours in September
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SLIDE 28

Spectrum: 950~1420 MHz

First HI cube covering the entire 0 < z < 0.5 range

1000 1100 1200 1300 1400

Frequency (MHz) mJy/beam

4 2

  • 2
  • 4

1400

z 0.5 0

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SLIDE 29

Frequency dithering

6-hour run

1000 1100 1200 1300 1400

Frequency (MHz) mJy/beam

4 2

  • 2
  • 4

1400

mJy/beam Frequency (MHz)

1000 1100 1200 1300 1400 1000 1000 4 2

  • 2
  • 4

3 frequency settings combined (18 hours)

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SLIDE 30

Verification

Frequency (MHz) 1340 1350 1360 1370 1380 1390 1400 1410 mJy/beam

0.2 0.1

  • 0.1
  • 0.2

Brightest detection in the pilot

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SLIDE 31

In a few years...

To Do:

  • 1. Observe 1002 hours to get HI images of these galaxies
  • 2. Pointed observations with ALMA for a subset of these in different environments and z