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A P E RT I Fimaging surveysMarc Verheijen9th PHISCC, Cape Town, 1-3 Feb 2016

A P E RT I Fimaging surveys Apertif specs & performanceHI science incentivesSurveys designSynergies and ancillary dataSurvey operations and science exploitation9th PHISCC, Cape Town, 1-3 Feb 2016

a grand proposalWSRT upgrade - SKA pathfinderAfter 45 years of service, transform theWSRT into an efficient 21cm surveyfacility using phased-array technology.APERTIFMFFE# antennas/dish!1212# primary beams!371field-of-view[deg2]80.3freq. range[GHz] 1.13 1.75 0.12 8.7Tsys[K]7030aperture efficiency!75%55%bandwidth[MHz]300160# channels!245761024# dishes1214 (13)(Aeff/Tsys)2 MFFE 14 4x (Aeff/Tsys)2Apertif 12APERTIF Resolution :Θ (1 Z)2x 15”x15”/sin(δ)(10kpc @ D 150 Mpc)R (1 Z) x 2.6 km/sAPERTIF increases surveyspeed of WSRT 20x9th PHISCC, Cape Town, 1-3 Feb 2016

HI mass limits & detection ratesBased on Alfalfa HIMF1x12hr : M*HI at z 0.08, 1x1011 Msun at z 0.2512x12hr : M*HI at z 0.16, 3x1010 Msun at z 0.259th PHISCC, Cape Town, 1-3 Feb 2016

HI column density limits5σ, W 25 km/sNote: smoothing to half the angular resolution reducesthe survey volume at a particular linear resolutionby a factor 8 .9th PHISCC, Cape Town, 1-3 Feb 2016

Inventory of community interestBased on input via Expressions-of-Interest:‣‣‣‣‣shallow northern-sky survey (SNS)medium-deep survey (MDS)pulsar/transients survey (PTS)Galactic plane survey (GPS)commensal transients search survey20 years of survey time requested9th PHISCC, Cape Town, 1-3 Feb 2016

Inventory of community interestBased on input via Expressions-of-Interest:‣‣‣‣‣shallow northern-sky survey (SNS)medium-deep survey (MDS)pulsar/transients survey (PTS)Galactic plane survey (GPS)commensal transients search surveyRealistic: 4-year survey period (2017 2020), 15% DD time,75% observing efficiency, ¼ of time dedicated to a survey 6600hr 550x12hr per surveyAmbitious : full northern-sky survey (10,000 deg2)9th PHISCC, Cape Town, 1-3 Feb 2016

Gas & Galaxy Evolution - resolved HI studiesFueling the Blue CloudSancisi 2008sustaining star formationbuilding up stellar massMergers / cold accretionand/orGalactic Fountain / Fallback ?Oosterloo 2007M 101SKA-SA, Cape Town, 28 Jan 2015

Gas & Galaxy Evolution - resolved HI studiesIllustris,Vogelsberger ’12Fueling the Blue CloudSancisi 2008sustaining star formationbuilding up stellar massMergers / cold accretionand/orGalactic Fountain / Fallback ?Oosterloo 2007M 101SKA-SA, Cape Town, 28 Jan 2015

Science requirement :minNHI 5x1019Accretion, depletion and removal of gastidal strippingram-pressure strippingOosterloo et alFraternali et alextra-planar gasVerheijen et al2x1019 (atoms/cm2)5x1019 (atoms/cm2)10x1019 (atoms/cm2)Gas disks are responsive to environmental influencesand reveal processes not easily observed otherwise.9th PHISCC, Cape Town, 1-3 Feb 2016

HI absorption studies1 in 3 continuum sources have associated HI absorptionFWHM 100 km/s100 km/s FWHM 200 km/sFWHM 200 km/sGereb ‘14High-velocity outflows from AGNsRequires astable bandpass.Morganti 9th PHISCC, Cape Town, 1-3 Feb 2016

OH megamasersidentify sites of intense star formationDarling & Giovanelli, 2003detectable at higher redshifts - trace cosmic evolution of major mergers.1430-1130 MHz 0.17 Z 0.47 for OH9th PHISCC, Cape Town, 1-3 Feb 2016

Apertif draft surveysGuiding principles:‣ public, legacy-type surveys (archival science)based on ideas from 18 Expressions-of-Interest ‣‣‣‣‣maximum ancillary data availabilitycommunity involvement & commitmentcollaborate, compromise, consolidatebe ambitious yet realisticsimplicityfew observing modes, fixed pointing grid‣ staged delivery of data and science9th PHISCC, Cape Town, 1-3 Feb 2016

Apertif survey definitionJuly 2015:Draft Survey ProgrammeGround Rules for involvement(surveys to be carried out by the community)!Apertif Survey Team: Tom Oosterloo (ASTRON/Groningen)! Raffaella Morganti (ASTRON/Groningen)! Erwin de Blok (ASTRON)! Thijs van der Hulst (Groningen)! Joeri van Leeuwen (ASTRON/Amsterdam)! Lister Staveley-Smith (UWA/ICRAR)!/ Gyula Jozsa (SKA-SA)! Marc Verheijen (Groningen)! January 2016: Apertif Survey Plan (under review)9th PHISCC, Cape Town, 1-3 Feb 2016

Apertif Survey PlanThree imaging and one pulsar/transients surveys : Shallow (1x12hr), large-area ( 3500 deg2) imagingoverlap with SDSS, PanStarrs-I, MaNGA, Califa, HetDex, S4G! Medium-deep (Nx12hr), medium-area ( 350 deg2) imagingoverlap 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 positionsAll surveys combined should result in an uniform LST coverage.9th PHISCC, Cape Town, 1-3 Feb 2016

Synergy - MaNGAA SDSS-IV multi-IFU survey of 104 nearby galaxies at z 0.03‣ 2” fibers‣ 17 IFU’s per 7 deg2 field‣ 12” 32” FoV per IFU‣ 360-1000 nm‣ R 20009th PHISCC, Cape Town, 1-3 Feb 2016

Apertif Survey PlanMaNGA fieldsCalifa pointings9th PHISCC, Cape Town, 1-3 Feb 2016

Synergy - Herschel-Atlas1/12th of NGP field, including ComaBlind Herschel PACS/SPIRE imaging ofNorth Galactic Pole region ( 150 deg2)PACS:110, 170 μmSPIRE: 250, 350, 500 μmGALEXSDSSUKIRT 500 sources/deg2Θ 18” at 250 μmSpitzer / WISEComplete SED reconstruction:‣ Total energy output‣ Star Formation Rates‣ Dust masses and temperaturesHerschelAll data arepublicly available.9th PHISCC, Cape Town, 1-3 Feb 2016

Synergy - HETDEXA blind IFU surveyusing VIRUS on HET22% fill factor over 300 deg2‣ 1.5” fibers‣ 448 fibers/IFU, 78 IFUs‣ 350-550 nmLy-α : Z 1.9 3.5[OII] : Z 0 0.48Hβ : Z 0 0.13[OIII] : Z 0 0.10‣ R 70016 arcmin 105 [OII] redshifts in Apertif bandwidth (Z 0.25)50” spacing9th PHISCC, Cape Town, 1-3 Feb 2016

Synergy - LOFARConfusion-limited continuum maps by Apertifwill detect the same star forming galaxies as LOFAR.7 μJy 1.2 GHz map higher-resolution LOFARmaps will facilitate sourceidentification! distinguish SF galaxies fromsteep-spectrum sourcesAlso:‣ galaxy cluster radio halos‣ radio relics‣ SKA-SA, Cape Town, 28 Jan 2015

Apertif Survey Plan Shallow Northern SurveyMedium-Deep SurveyLOFAR fields H-AtlasHETDEXCVnPointing grid andsurvey boundarydetails to bedetermined.Perseus-Pisces9th PHISCC, Cape Town, 1-3 Feb 2016

Apertif survey operationsTwo observing modes: imaging in maxi-short configuration transient searches in Nx144m configurationEach configuration is operational for weeks/monthsApertif Survey Team (i.e. the community) is responsible for :‣ Scheduling observations‣ Quality Assessment‣ Flagging, calibration and analysis of data‣ Delivery of data products into archive‣ PublishingDaily operations by Survey Astronomers on Duty (SADs)provided by AST members (students, postdocs, faculty).SKA-SA, Cape Town, 28 Jan 2015

Data products & Data releasesGoal : legacy value of survey data through Long-Term ArchiveThe AST is responsible for:Level 0 : quality-controlled raw visibilities ( 1 TB/12hr)Level 1 : flagged and calibrated visibilities (tables)Level 2 : continuum-subtracted line cubes and cont./pol. imageThe SWGs are responsible for :Level 3 : source catalogs (positions, redshifts, fluxes, line widths )Level 4 : higher order products (HI maps, vel. fields, RM cubes )Level 5 : science-specific products (mass models, kin. analysis )Annual data releases after proprietary periods.SNS : 6 months after final observation of previous yearMDS : survey uniformity determines release scheduleSKA-SA, Cape Town, 28 Jan 2015

Scientific exploitation of Apertif surveysProject-based and carried out by SWGs under auspices of the AST.Each SWG has a representative on the AST and may consist of several Individual Researchers (e.g. students/postdocs) and/or Project Teams focussing on a particular topicEach IR/PT within a SWG provides a focused and realistic research plan a timeline of activities a publication plan an overview of data products to be generatedThe AST monitors and coordinates activities of SWGs to avoidconflicts of interest and to protect student projects.SKA-SA, Cape Town, 28 Jan 2015

Summary & OutlookTwo observing modes (imaging and transients)Two imaging depthsSurvey areas driven by science (synergies) and efficiencySurvey operations done by the community!Mar - Jul : tech. and sci. commissioning with limited arrayAugust : full array available for early sciencemid 2017 : start of surveys through 2020SKA-SA, Cape Town, 28 Jan 2015

9th PHISCC, Cape Town, 1-3 Feb 2016 Inventory of community interest ‣ shallow northern-sky survey (SNS) ‣ medium-deep survey (MDS) ‣ pulsar/transients survey (PTS) ‣ Galactic plane survey (GPS) ‣ commensal transients search survey Based on input via Expressions-of-Interest: Realistic: 4-year survey period (2017 2020), 15% DD time,