Six of the 36 ASKAP dishes (photo by Maxim Voronkov ......HI in the NGC 3263galaxy group –...
Transcript of Six of the 36 ASKAP dishes (photo by Maxim Voronkov ......HI in the NGC 3263galaxy group –...
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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
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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)
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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
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Baerbel Koribalski * HI Early Science with ASKAP-ADE12 HI in the NGC 3263 galaxy group – English, BK et al. (2010)
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 science goal for ASKAP-ADE12
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Baerbel Koribalski * HI Early Science with ASKAP-ADE12 HI in the NGC 3263 galaxy group – English, BK et al. (2010)
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 !
Our science goal for ASKAP-ADE12
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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.
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Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
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)
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Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
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
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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
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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
slide by Barbara Catinella
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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)
slide by Barbara Catinella
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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”
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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
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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
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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
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ASKAP status recent achievements
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BETA Mk1 PAFs – an engineering testbed
Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
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
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one ADE PAF installed ? system test under way Tsys measured: 50 K ?
by end of this year ?
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Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
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
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by end of 2014 ?
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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.
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Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
M83 Group
5o
ATCA primary beam
HIDEEP – mom0 map
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Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
M83 Group
5o
ATCA primary beam
HIDEEP – mom0 map
ASKAP large field-of-view
demonstrator science
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* ReUre Mk1 PAFs * allow installaUon of ADE PAFs 7-‐12 on inner-‐most ASKAP antennas to achieve short baselines (ASKAP Change Request submiYed)
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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
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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
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• 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
Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
Study the evolution of galaxies, their transformation and star formation as a function of environment.
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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
Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
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
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• 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
Baerbel Koribalski * HI Early Science with ASKAP-‐ADE12
• syn. beam 20”-‐30” (6” pixels?) • 16384 channels, each 18.5 kHz • keep visibiliTes unTl imaging is
complete
• shared risk observing
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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.