WEAVE-WEAVE-ApertifApertifJesús Falcón-Barroso

many thanks to Marc Verheijen

ApertifApertif@WSRT@WSRT

● Apertif is the first working focal-plane array capable of full Westerbork resolution (~15”x15” beam) over a single, full 8 deg2 pointing

● Operating in the frequency range 1000-1750 MHz with nearly the sensitivity of the present single-pixel WSRT frontend

● With Apertif, the WSRT can image an area on the sky about 25 times the size of the full moon.

ApertifApertif Science Science

● Neutral hydrogen surveys - emission & absorption from the smallest to the most distant galaxies

● Radio continuum surveys - Synergy with LOFAR● Pulsar searches● Magnetic fields in the Milky Way and other galaxies● (extra)galactic OH (mega-)masers ● Radio Recombination Lines● Variables and Transient sources● Search for Extra-Terrestial Intelligence

ApertifApertif Survey Survey

Apertif will consist of three imaging and one pulsar/transient surveys:

● Shallow (1x12hr), large area (3500 deg2) imaging overlap with SDSS, PanStarrs-I, MaNGA, Califa, HetDex, S4G

● Medium-deep (Nx12hr), medium-area (~350 deg2) imaging overlap with H-Atlas+Coma, CVn, HetDex, Perseus-Pisces

● Apertif-LOFAR (4x12hr, ~10 fields of 10 deg2) imaging

● Wide-field pulsar and transients survey (3hr, 15.000 deg2) triggers LOFAR for accurate FRB positions

All surveys combined should result in homogeneous LST coverage

ApertifApertif “Footprint” “Footprint”

● 105 HI detections and 104 resolved HI disks

ApertifApertif “Footprint” “Footprint”

● It will provide resolved HI data up to z=0.26

Synergy with WEAVESynergy with WEAVE

● Provide a broader astrophysical context for HI detections

● Apertif provides resolved HI observations over a large FoV for many thousands of galaxies

● WEAVE provides the optical component on similar scales with the LIFU mode

● It allows for a different way to define galaxy samples(based on resolved HI observations, not on optical obs.)

● WEAVE-Apertif offers a combination of Optical+HI observations not possible with other ongoing IFU surveys(e.g. large spatial coverage with high spectral resolution)

WEAVE-WEAVE-ApertifApertif Science Science

Open questions to be addressed with WEAVE-Apertif:

The nature of galaxy bimodalityThe nature of galaxy bimodality● Why is there a bimodality in galaxy properties today, such that there are both

star-forming blue galaxies and red, dead galaxies? ● Where does the gas fuelling the star formation in these galaxies come from? ● How is the star formation shut down?

Disk galaxy mass dissectionDisk galaxy mass dissection● How much dark matter do disc galaxies have?● How is it distributed?

Secular evolution of galaxiesSecular evolution of galaxies● What's the process driving radial migration of stars?● What's the level of scattering and radial motions induced by spiral arms and

bars in stars?● What's the impact of accretion of satellites in the chemo-dynamical

properties of galaxies?● How does it all connect with observations in the Milky Way?

The nature of galaxy bimodalityThe nature of galaxy bimodality

Fueling of the MSFueling of the MSSustaining SF

Build-up of stellar mass-

Mergers/AccretionGalactic fountain/fallback

Examples from Sancisi et al. (2008)

Faber et al.

SF quenchingSF quenching

External agents:Tidal strippingRam-pressure

Internal origin:AGN

Starburst driven

The nature of galaxy bimodalityThe nature of galaxy bimodality

Inter-galactic HI in groups Ram-pressure stripping

NGC2146

Kreckel et al. (2014)

Disk galaxy mass dissectionDisk galaxy mass dissection

Kinematics of Low Surface Brightness galaxies

HI

HαHα+HI rotation curve

Sw

ate

r s e

t al (2

003)

Disk galaxy mass dissectionDisk galaxy mass dissection

Mapping ionised gas kinematics at z~0.2

HI detection at z=0.188

[OII] velocity field

PMAS 16”x16” FoV3.5m@CAHA

Secular evolution of galaxiesSecular evolution of galaxies

● Highly detailed studies of stellar, ionised gas and HI content of large nearby spirals

● Galaxies with large amounts of ancillary imaging and spec. data (e.g. CO, GALEX, Spitzer)

HALOGAS Survey

Secular evolution of galaxiesSecular evolution of galaxies

Kamphuis & Brigs (1992)

NGC628

19 WEAVE-LIFU pointingsPrevious attempts with PPaK required 34 pointings as part of PiNGS survey (Sánchez et al. 2011, Sánchez-Blázquez et al. 2014)

Hα Age [M/H]

WEAVE-WEAVE-ApertifApertif Survey plan Survey plan

A three-tiered survey over ~350 nights:● Tier 1: LIFU of ~5000 Apertif resolved galaxies● Tier 2: LIFU of ~50 LSB galaxies + mIFU of high surf.bright.

galaxies at z~0.25● Tier 3: 4 nights/galaxy with LIFU for ~10 nearby, large galaxies

Low-res mode: mIFU (R~5000, D=1.3”), LIFU (R~2500, D=2.6”)● Ionised-gas kinematics● Evolutionary state of the stellar populations● ISM & star formation properties

High-res mode: mIFU (R~20000, D=1.3”), LIFU (R~10000, D=2.6”)● Stellar kinematics, disk dynamics (MgI, CaT lines)● Ionised-gas kinematics

● Low-res wavelength range: 3660–9840Å● High-res wavelength range: 4040–4650Å, 4730–5450Å, 5950–6850Å

Synergies with WEAVE surveysSynergies with WEAVE surveys

Scientific level:● Clusters● STEPS● Galactic Archaeology● SCIP● M31 and M33

Operational level:● Clusters● LOFAR

Break-Out sessionBreak-Out session(Elton room)(Elton room)

● Welcome / Goal of the session● Apertif survey status/update (Kelley Hess)● Main science topics currently proposed● Outcome of Survey Strategy Review● New science topics?● Recap of instrumental specifications● Team structure / People involvement● Next steps / Planning