six of the 36 askap dishes (photo by maxim voronkov ......hi in the ngc 3263galaxy group –...

CSIRO Astronomy and Space Science

Six of the 36 ASKAP dishes (photo by Maxim Voronkov, CASS)

Australian SKA Pathfinder (0.7 - 1.8 GHz)

HI Early Science: se9ng the scene from now to ASKAP-‐12 and beyond

HI Early Science: se9ng the scene from now to ASKAP-‐12 and beyond

CSIRO Astronomy and Space Science

Hydrogen as a tracer of tidal interactions (Putman et al. 1998)

Baerbel Koribalski * HI Early Science with ASKAP-ADE12 HI in the NGC 3263 galaxy group – English, BK et al. (2010)

Study the evolution of galaxies, their transformation and star formation as a function of environment.

Our science goal for ASKAP-ADE12


Study the HI morphology, kinematics and star formation of galaxies in:

•  voids (slides by B. Catinella)

•  loose groups (slides by V. Kilborn)

•  compact groups •  and clusters (slides by L. Cortese)

Discover HI clouds / filaments between galaxies, tracing their interaction history.



Our strategy:

•  in-depth study of 10 fields (z = 0 – 0.2) •  targeting galaxies in different environments •  approx. 60 hours (6-10 nights) per field •  need to resolve galaxies and detect faint gas

in and outside galaxy disks •  focus on nearby groups and clusters

See talk by Tobias Westmeier !


Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12

VLA HI Study of the Virgo Cluster.

About 400h to obtain single pointings of 53 late-type Virgo cluster galaxies.

SDSS + HI contours (Chung et al. 2009).

5o

Groups & Cluster are excellent targets to study the

physical processes that disrupt and transform galaxies

in a medium to high density environment. Galaxy HI

morphologies and kinematics are strongly affected.


The 21-cm spectral line allows us to study

•  the physical processes affecting galaxy disks •  star-formation locations in the outer disk •  gaseous filaments/bridges between galaxies •  intra-group/cluster gas

SDSS + HI contours (Chung et al. 2009) HI distribution (Oosterloo & vG 2005)


The 21-cm spectral line allows us to study

•  the physical processes affecting galaxy disks •  star-formation locations in the outer disk •  gaseous filaments/bridges between galaxies •  intra-group/cluster gas

SDSS + HI contours (Chung et al. 2009)

HI in Ursa Major: S0 galaxy NGC 4111

Verheijen & Zwaan 2001 Wolfinger et al. 2013 Picture by Martin Pigh (Yass, NSW), winner of the

2013 David Malin Astrophotography Competition.

The warped spiral galaxy NGC 3718

HI imaging of galaxies in voids

Voids are not empty! J Why they are interesting places to look at: u  Galaxy evolution least affected by environment u  Best (?) places to look for ongoing gas accretion u  Test ΛCDM cosmology (predicted numbers and location of low-mass halos in

voids not consistent with optical observations) u  Never surveyed systematically (with enough sensitivity) in HI… expect surprises!!

Examples of galaxies located in the deepest regions of local voids, observed with WSRT (Kreckel et al 2012): HI masses = 1.7 x 108 – 5.5 x 109 M¤

slide by Barbara Catinella

Phoenix/Eridanus Void: a suitable target for ASKAP12

R.A.=1.5 hr, DEC=-50 deg, cz=3000 km/s (~43 Mpc; SSRS1, da Costa et al 1988) size ~ 30 x 30 x 40 Mpc, behind Fornax Cluster RA vs redshift

distribution of galaxies with

DEC~ -20 to -50 (Maurellis et al

1990)

cz

Fornax


ASKAP12 HI-blind void survey

u  Need a huge FOV to survey local voids à unique niche for ASKAP!! u  Ideally, survey from the center of the void to the edge, sampling a range of

density environments. For a pilot, target a couple of fields (center and edge) u  Need to be able to get to HI masses of a few 108 M¤ If rms~5 mJy/beam in 8 hrs à MHI=1.2 108 M¤ (D=40 Mpc, unresolved, 10σ detection over Δv=40 km/s)


The Group environment: An excellent match for ASKAP-‐12

Parkes HI imaging of two loose groups

Unresolved HI (contours) and known galaxies (crosses)

Kilborn et al.

2005, 2006, 2009

ONE poinTng of ASKAP-‐12 would allow us to look at the morphology of all members of loose groups – an environment where galaxies are pre-‐processed. Look for signs of interacTons, mergers, ram pressure stripping and strangulaTon.

slide by Virginia Kilborn

Coordinator of the WALLABY SWG3

“Galaxy Environments”

HI deficient

HI excess Using HI maps to

determine the morphology of HI deficient and HI excess galaxies: HI stripping and

HI accreTon methods in spiral galaxies

HI deficient HI deficient

Kilborn et al.

Denes et al.

slide by Virginia Kilborn

HI across environment today

Galaxy Density

Sta

r F

orm

atio

n R

ate

Lewis et al. 2002

Star formation strong function of environment

What about gas? How is cold gas affected by

environment?

With current facilities we can only investigate the two extremes: i.e., cluster / isolation

?

slide by Luca Cortese

Lewis et al. 2002

HI across environment with ASKAP12 Unveiling cluster infalling regions and groups: where most of the action is taking place!

Cluster Filaments

Ideal Target for ASKAP-12: Fornax and the filaments feeding it

•  Close to us (~16 Mpc) •  Size Matches perfectly ASKAP FoV •  At the intersection of LS filaments •  ALL density scales with a few pointings

slide by Luca Cortese

Scott et al. 2012

ASKAP status recent achievements

BETA Mk1 PAFs – an engineering testbed


3 & 9 beam conTnuum images achieved with 3 PAFs

3 beams

BW = 16 x 1 MHz 12h, 1p, 928 MHz

9 beams

BW = 32 x 1 MHz 12h, 1p, hardware corr.

Parkes multibeam

BW = 64 MHz (1024 ch) 8 min/pointing, 2 pols 15.5 arcmin resolution

HIPASS 20-‐cm radio conTnuum map

one ADE PAF installed ? system test under way Tsys measured: 50 K ?

by end of this year ?


BETA = 5-‐6 Mk1 PAFs working together producing 9-‐beam conTnuum maps + HI images/spectra for science verificaTon

The starburst galaxy NGC 253 is a member of the Sculptor Group. It has ~6 Jy radio continuum flux at 20-cm; very bright HI emission (and absorption) over 400 km/s, approx. from 1418 - 1420 MHz.

NGC 253

HIPASS spectrum

by end of 2014 ?

Six ADE PAFs working together could produce this:

Atomic Hydrogen in the LMC (Kim et al. 1998)

Infrared Portrait of the LMC (Spitzer + Herschel)

Large field-of-view demonstrator science.


M83 Group

5o

ATCA primary beam

HIDEEP – mom0 map


M83 Group

5o

ATCA primary beam

HIDEEP – mom0 map

ASKAP large field-of-view

demonstrator science

* ReUre Mk1 PAFs * allow installaUon of ADE PAFs 7-‐12 on inner-‐most ASKAP antennas to achieve short baselines (ASKAP Change Request submiYed)

BETA / ASKAP Early Science Fields

Baerbel Koribalski * HI Early Science with ASKAP-ADE12

ASKAP-ADE 6 – 12+ dishes

PAF field-of-view (30 sq deg)

Moon to scale

Circinus field: isolated nearby galaxy

BETA / ASKAP Early Science Fields

Baerbel Koribalski * HI Early Science with ASKAP-ADE12

ASKAP-ADE 6 – 12+ dishes

PAF field-of-view (30 sq deg)

Moon to scale

Fornax field: a nearby galaxy cluster

•  ASKAP-‐ADE12 HI line sensiTvity and configuraTon studies (WALLABY Memos 13 & 14; Tobias Westmeier et al.)

•  HI Early Science – our “umbrella theme”:

•  Approx. 10 target fields – observe for ≥60 hours each (resulTng in HI line rms per 4 km/s channel of ~1.6 mJy/beam and angular resoluTon of ~20-‐30 arcsec)

ASKAP-‐12 HI Early Science


Study the evolution of galaxies, their transformation and star formation as a function of environment.

ASKAP-‐ADE12 HI survey speed ≥ VLA HI survey speed

(assuming ASKAP-‐ADE Tsys = 50 K @ 1.1 -‐ 1.4 GHz, efficiency η = 0.8)

HI Spectral Line SensiUvity


Time on source to reach an rms of 4-‐5 mJy/beam

Mapped area for 8 hour integraUon reaching an rms of 4-‐5 mJy/beam

ATCA 50 minutes 9-‐point HI mosaic (pbeam ~ 34’)

VLA 10 minutes 48-‐point HI mosaic (pbeam ~ 30’)

ASKAP-‐ADE12 480 minutes PAF field-‐of-‐view (≈30 sq degr) eq to 36-‐point HI mosaic (pbeam ~ 63’)

ASKAP-‐ADE30 74 minutes 6.5 PAF fields

•  Each field: ≈60h on-‐source, ie about 6-‐10 nights observing Ø  dither or choose offset poinTng posiTon each night (Nyquist sample)

•  FOV ≈ 30 sq degr (approx. 5.5 degr x 5.5 degr)

ASKAP-‐12 HI ObservaUons


•  syn. beam 20”-‐30” (6” pixels?) •  16384 channels, each 18.5 kHz •  keep visibiliTes unTl imaging is

complete

•  shared risk observing

CSIRO Astronomy and Space Science * Contact: [email protected]

Target ~10 fields ≥ 60 h each Umbrella Theme: Galaxy evolution as a function of environment. How do physical processes affect the HI morphology and kinematics of galaxies in voids, groups & clusters.

Contributors: BK, Lister, Tobias, Ivy, Virginia, Barbara, Luca, et al.

six of the 36 askap dishes (photo by maxim voronkov ......hi in the ngc 3263galaxy group –...

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