1. MeerKAT MIGHTEE Survey Ancillary Data Needs/Plans Mattia Vaccari http://www.mattiavaccari.net SKA SA Fellow, UWC On behalf of Kurt van der Heyden & Matt Jarvis SALT/MeerKAT Workshop MeerKAT Office - Cape Town - 05 Nov 2012

2. Filipe Abdalla (UCL, UK), Jose Afonso (Lisbon, Pt), Vinod Arumugam (ATC, UK), David Bacon (Portsmouth, UK), Manda Banerji (Cambridge, UK), Bruce Bassett (UCT, SA), Richard Battye (Manchester, UK), Werner Becker (MPE, Germany), Girish Beeharry (Univ. Mauritius, Mauritius), Philip Best (Edinburgh, UK), Rob Beswick (Manchester, UK), Michael Bietenholz (HartRAO/York, SA/Canada), Dave Bonfield (Hertfordshire, UK), Malcolm Bremer (Bristol, UK), Michael Brown (Monash, Au), Michael Brown (Cambridge, UK), Shea Brown (CSIRO, Au), Ian Browne (Manchester, UK), Marcus Bru ̈ ggen (Jacobs University, Germany), Scott Chapman (Cambridge, UK), Chris Clarkson (UCT, SA), Marcel Clemens (INAF, It), Pieter Conradie (NASSP, SA), Chris Conselice (Nottingham, UK), John Conway (Chalmers, Sweden), Kristen Coppin (Durham, UK), Garret Cotter (Oxford, UK), Steve Crawford (SAAO, SA), Catherine Cress (UWC, SA), Simon Cross (MeerKAT, SA), Erwin De Blok (UCT, SA), Okkie De Jager (NWU, SA), Roger Deane (Oxford, UK), James Dunlop (Edinburgh, UK), Loretta Dunne (Nottingham, UK), Ed Elson (UCT, SA), Andreas Faltenbacher (UWC, SA), Ilana Feain (CSIRO, Au), Chiara Ferrari (OCA, France), Luigina Feretti (INAF, It), Tony Foley (MeerKAT, SA) Bradley Frank (UCT, SA), Bryan Gaensler (Sydney, Au), Mike Garret (ASTRON, NL), Jim Geach (Durham, UK), Gabriele Giovannini (INAF, It), Eduardo Gonzalez-Solares (IoA, Cambridge), Dave Green (Cambridge, UK), Martin Hardcastle (Hertfordshire, UK), George Heald (ASTRON, NL), Nalini Heeralall Issur (Univ. Mauritius, Mauritius), Ian Heywood (Oxford, UK), Matt Hilton (UKZN, SA), Renee Hlozek (Oxford, UK), Benne Holwerda (UCT, SA), Andrew Hopkins (AAO, Au), Cathy Horellou (Chalmers, Sweden), Jasper Horrel (MeerKAT, SA), Minh Huynh (IPAC, USA), Hans-Rainer Klo ̈ ckner (Oxford, UK), Roger Ianjamasimanana (UCT, SA), Eduardo Ibar (ATC, UK), Rob Ivison (ATC, UK), Neal Jackson (JB, UK), Justin Jonas (MeerKAT, SA), Louise Ker (Edinburgh, UK), Alexei Kniazev (SALT, SA), Anton Koekemoer (STScI, USA), Rene ́e Kraan-Korteweg (UCT, SA), Jean-Claude Kubwimana (UCT, SAAO, SA), Koen Kuijken (Leiden, NL), Mark Lacy (NRAO, USA), Nicola Loaring (SAAO, SA), Ilani Loubser (NWU, SA), Stuart Lumsden (Leeds, UK), Roy Maartens (Portsmouth, UK), Gordon Macleod (DST, SA), Steve Maddox (Nottingham, UK), Bryony Martin (NASSP, SA), Ross McLure (Edinburgh, UK), Richard McMahon (Cambridge, UK), Pieter Meintjies (UFS, SA), Hugo Messias (Lisbon, Portugal), George Miley (Leiden, NL), Kavilan Moodley (UKZN, SA), Raffaella Morganti (ASTRON, NL), Eric Murphy (Caltech, USA), Ray Norris (CSIRO, Au), Nadeem Oozeer (HartRAO, SA), Se Heon Oh (UCT, SA), Patrice Okouma (UCT, SA), Seb Oliver (Sussex, UK), Darragh O’Donoghue (SAAO, SA), Bob Osano (UCT, SA), Viral Parekh (UCT, SA), Prina Patel (Portsmouth, UK), Chris Pearson (RAL, UK), Nikki Pekeur (UNW, SA), Mirjana Povic (IAC/UKZN, Sp/SA), Isabella Prandoni (INAF, It), Alvise Raccanelli (Portsmouth, UK), Dinesh Radhakhrishna (Univ. Mauritius, Mauritius), Steve Rawlings (Oxford, UK), Somak Raychaudhury (Birmingham, UK), Marco Regis (UCT, SA), Laura Richter (MeerKAT, SA), Dimitra Rigopoulou (Oxford, UK), Encarni Romero Colmenero (SALT, SA), Huub Ro ̈ ttgering (Leiden, NL), Lawrence Rudnick (UMN, USA), Mario Santos (UTL, Portugal), Anna Scaife (Dublin, Ireland), Anja Schro ̈ der (MeerKAT, SA), Ramotholo Sefako (SAAO, SA), Stephen Serjeant (OU, UK), Nick Seymour (MSSL, UK), Muzikayise Sikhonde (NASSP, SA), Chris Simpson (LJMU, UK), Bruce Slee (CSIRO, Au), Ian Smail (Durham, UK), Anthony Smith (Sussex, UK), Mathew Smith (UCT, SA), Ian Stewart (UCT, SA), Jeroen Stil (Calgary, Canada), Kim Sung (Sejong, Korea), Yabebal Tadessa (SISSA, It), Russ Taylor (Calgary, Canada), Petri Vaisanen (SALT, SAAO, SA), Melvin Varughese (UCT, SA), Mattia Vaccari (Padova, It), Nic Walton (Cambridge, UK), Aprajita Verma (Oxford, UK), Amanda Weldman (UCT, SA), Glenn White (OU, UK), Eric Wilcots (Wisconsin, USA), Richard Wilman (Swinburne, Au), Hartmut Winkler (UJ, SA), Patrick Woudt (UCT, SA) The MIGHTEE Team Kurt van der Heyden (UCT) & Matt Jarvis (Oxford/UWC)

3. Key Science of MIGHTEE The Evolution of Star-formation activity across cosmic time  Philip Best (Edinburgh), Seb Oliver (Sussex) The Evolution and impact of AGN activity over cosmic time  Martin Hardcastle (Herts), Isabella Prandoni (Bologna), Chris Simpson (LJMU), Matt Jarvis (Ox/UWC) Galaxy Clusters and Galaxy evolution in dense environments  Marcus Bruggen (Jacobs), Ian Smail (Durham) Cosmology and LSS  Matt Jarvis (Ox/UWC), Catherine Cress (UWC), David Bacon (Ports) HI and OH absorption studies  Hans-Rainer Klockner (Bonn/Ox), Rob Beswick (Mancs) The Polarized Sky  Anna Scaife (Dublin), Russ Taylor (Calgary), Richard Battye (Mancs)

4. The MeerKAT International Giga-Hertz Tiered Extragalactic Exploration (MIGHTEE) Survey Kurt van der Heyden (UCT) & Matt Jarvis (Oxford/UWC)

6. EMU

7. MIGHTEE-1 MIGHTEE-3 MIGHTEE- 2 EMU

8. MIGHTEE-1 MIGHTEE-3 MIGHTEE-2 EMU

9. Courtesy of Seb Oliver

10. MIGHTEE Fields Tier-3/4 : LADUMA Commensal Observing in CDFS Spec-Z Follow-Up Planning Underway (See Sarah’s Talk) Tier-2 : COSMOS / ELAIS-S1 / XMM-LSS / CDFS 35 deg 2 overall i.e. ~10 deg 2 / field

11. MIGHTEE Fields Tier-3/4 : LADUMA Commensal Observing in CDFS Spec-Z Follow-Up Planning Underway (See Sarah’s Talk)

12. MIGHTEE Fields Tier-2 : COSMOS / ELAIS-S1 / XMM-LSS / CDFS 35 deg 2

13. Multi-Wavelength Synergies Optical (CFHTLS, SXDS, VST-VOICE, DES) NIR (UKIDSS-UDS, VISTA-VIDEO) MIR/FIR : Spitzer (SWIRE/SERVS/S-COSMOS) FIR/SMM : Herschel (HerMES/PEP) & SCUBA2 CLS

14. ” It will be like being on the Moon and being able to recognize buildings in New York and trucks on Broadway" Nick Scoville, 2003 The COSMOS Field Widest-Area (2 deg 2 ) HST Imaging Survey 30-band Deep Photometry (And UltraVISTA Field)

15. The VIDEO Survey Fields (PI : Jarvis) (Jarvis et al. 2012, arXiv:1206.4263) Filter Time (per source) Time (full survey) 5  AB 5  Vega UKIDSS- DXS Seei ng Moon Z17.5 hours456 hours25.725.2-0.8D Y6.7 hours175 hours24.624.0-0.8G J8.0 hours209 hours24.523.722.30.8G H8.0 hours221 hours24.022.7220.8B KsKs 6.7 hours180 hours23.521.720.80.8B ECDFS XMM-LSSELAIS-S1

16. VIDEO Photometric Redshifts (Jarvis et al. 2012, arXiv:1206.4263) Galaxie s AGNs K [AB] < 23.5 (0.7 deg 2 ) K [AB] < 23.5 (0.7 deg 2 ) Photometric Redshifts combining CFHTLS- D1/VIDEO High Source Density of High-Redshift Galaxies & AGNs [eventually over ten(s of?) square degrees]

17. VST Imaging Surveys in MIGHTEE/VIDEO Fields K [AB] < 23.5 (0.7 deg 2 ) K [AB] < 23.5 (0.7 deg 2 ) gri Multi-Epoch for SN Search & AGN Variability Studies ugri Deep Stacks to be combined with VIDEO/SERVS Background Image : SERVS Coverage 2011/20122012/2013 2013/2014 VST-VOICE (PIs : Covone & Vaccari) ESO VST GT Survey 4+4 deg 2 in CDFS+ES1 in ugri to m AB ~26 1) image/site quality 2) u-band sensitivity 3) multi-wavelength

18. Dark Energy Survey in MIGHTEE/VIDEO Fields K [AB] < 23.5 (0.7 deg 2 ) DES Supernova Survey Fields (cf. LSST Deep Drilling) 2 Deep + 8 Shallow (Mostly MIGHTEE/VIDEO) Fields

19. The AGN luminosity function with MIGHTEE

20. The AGN luminosity function with MIGHTEE + EMU

21. The star-forming galaxy luminosity function with MIGHTEE

22. The star-forming galaxy luminosity function with MIGHTEE + EMU

23. Source confusion for 8km baselines

24. Whose (Very) Extended CDFS? ECDFS (0.25 deg 2 ) VST VOICE VISTA VIDEO SERVS (4.5 deg 2 ) SWIRE (7.5 deg 2 ) 1/2 deg radius

25. The (Very) Extended CDFS Extant Ancillary Data See Natasha’s comprehensive summary at http://www.ast.uct.ac.za/~nmaddox/Laduma/ ECDFS, CDFS SERVS, CDFS SWIRE ECDFS provides ‘ideal’ dataset to compare against CDFS SERVS Opt/NIR Phot Surveys Ongoing/Planned Must actively pursue Spec Surveys outside ECDFS

26. CDFS SERVS SERVS VISTA- VIDEO VST-VOICE

27. CDFS SERVS Phot Data (5σ) GALEX DIS : FUV & NUV down to m AB ~24 VST-VOICE + DES : ugrizy to m AB ~26 VISTA-VIDEO : ZYJHK to m AB ~25.7/24.6/24/5.24/0/23.5 SERVS : Spitzer IRAC 3.6 & 4.5 μm to ~2 μJy SWIRE : Spitzer IRAC 5.8 & 8.0 μm to ~30 μJy SWIRE : Spitzer MIPS 24/70/160 μm to ~0.3/20/100 mJy HerMES : PACS 100/160 μm to ~30/60 mJy HerMES : SPIRE 250/350/500 μm to ~15 mJy ATLAS : ATCA 1.4 GHz Continuum to ~ 50 μJy

28. CDFS SERVS Spec Data ECDFS-only so far... Major recent efforts! NED - 1 k/deg2 CSI (Kelson+ 2012) - 5 k/deg 2 - i<23 - All Field (Spitzer) PRIMUS (Coil+ 2011) - 10 k/deg 2 - i<23 (Spitzer) ACES (Cooper+ 2012) - 20 k/deg 2 - R<24 (Optical)

29. Spectroscopic Survey Facilities (with Community Access) VIRUS@HET : HetDEX 300 deg 2 Survey ?? ngCFHT : Spec-Z Counterpart to CFHTLS ?? Subaru : WFMOS Complementing HyperSC ? VLT-MOONS : 300 deg 2 Public Survey ? VISTA-4MOST : 20,000 deg 2 Public Survey ?? DESpec : 5,000 deg 2 Proprietary Survey

30. MIGHTEE : SALT Role MIGHTEE will start when most major supporting multi-wavelength wide-field photometric surveys will either be completed or close to completion Wide-Field Multi-Object Spectroscopic Surveys, however, will hopefully be only about to get started In the meantime, there will be opportunities for several Non-MIGHTEE-specific follow-up projects (e.g. based on VOICE+DES/VIDEO) which will make effective use of versatile Optical/NIR spectrometers

31. SALT Faint QSO Follow-Up Program (Jarvis, Maddox et al., Approved Sep 20112) Exploiting UKIDSS-LAS/SDSS QSO Color- Color Selection Technique by Maddox et al. 2008 ~100 high-reliability QSO candidates over ~1 deg 2 Black Hole Mass vs Bulge Mass Relation at high z Faint-end slope of the QSO Luminosity Function Star Formation vs Black Hole Accretion Activity Paving the way for MeerKAT/MIGHTEE Science

32. A Wide-Field Multi-Object Spectrograph for SA(LT)? VIDEO can exploit available multi-wavelength data thanks to ground-breaking observing capabilities MIGHTEE will find itself in similarly favorable situation (Ability to observe all of the LSST Deep Drilling Fields) SA involvement in VOICE+DES/VIDEO will help Small SALT Observing Programs will soon ramp up, but Spectroscopic Redshifts for the bulk of MIGHTEE sources can only be obtained by dedicated instruments Opportunity for SA(LT) WFMOS vs Planned Facilities?