The SCUBA-2 Cosmology Legacy Survey and beyond Jim Geach on behalf - - PowerPoint PPT Presentation

The SCUBA-2 Cosmology Legacy Survey and beyond

Jim Geach on behalf of the S2CLS consortium

#SMG20 / Durham / 31st July 2017

Take home message

Please exploit the S2CLS data!

What is was the SCUBA-2 Cosmology Legacy Survey?

Largest of the JCMT Legacy Surveys: 65% of all SCUBA-2 time to be spent on JLS, over half this to be spent on CLS. PIs: Smail, Dunlop, van der Werf, Halpern. CLS (high redshift) 1778 hours 50.9% GBS (local star formation) 412 hours 11.8% SASSy (‘all/ambitious’ sky survey) 480 hours 13.8% NGLS (nearby galaxies) 100 hours 2.9% JPS (Galactic plane) 450 hours 12.9% SONS (stars) 270 hours 7.7% 3490 hours 291 nights

Operating in 450 and 850 micron windows simultaneously using two array(s) of superconducting TES bolometers Large format allows efficient large-area scanning (8 arcmin FoV ~ 10x SCUBA) See Holland et al. (2013) for comprehensive details

Simple two tier strategy covering well-known fields, observations 2011-2015

• Wide survey at 850um in grade 2-3 conditions (𝛖=0.05-0.12)
• Target area 10 deg2 (eventually completed ~5 deg2)
• Uniform coverage to 1-sigma=1.2mJy
• PONG mapping strategy
• Deep survey at 450um + 850um in grade 1 conditions (𝛖<0.05)
• Target area 0.25 deg2 over HST/CANDELS fields
• Uniform coverage 1sigma=1.2mJy @ 450um / confusion limited at 850um
• DAISY (point source) mapping strategy

What is was the SCUBA-2 Cosmology Legacy Survey?

Science drivers (and outputs)

• Comprehensive survey of SMGs detected at 850um over several ~degree scale fields
• measure environment / clustering / halo properties (Smail et al. 2014, Wilkinson et al. 2017)
• constrain bright-end counts, bright SMGs (Geach et al. 2017, Michałowski et al. 2017)
• reliably probe properties of SMGs (Chen et al. 2016)
• AGN/starburst connection (Banerji et al. 2015, Ramasawmy et al. 2017 in prep)
• evolution (Koprowski et al. 2016, Bourne et al. 2017)
• cross-correlation / stacking studies (Coppin et al. 2015, Koprowski et al. 2017 in prep)
• resolved follow-up (Simpson et al. 2015, 2017)
• ‘Keyhole’ confusion limited survey at 450+850um
• properties of 450um-selected SMGs below Herschel confusion limit (Roseboom et al. 2013)
• resolving CIB at 450um (Geach et al. 2013)
• probing faint end of counts (Zavala et al. 2017)
• joint stellar+dust+gas morphologies (HST-CANDELS overlap, ALMA follow-up ongoing)

20 years ago: our first glimpse of the submm (distant) Universe, with SCUBA (Smail et al. 1997, Barger et al. 1998, Hughes et al. 1998)

Hughes et al. (1998) The HDF

Borys et al. (2003)

~1 ~10 years ago: ‘pr prope per’ submm su surve veys ys

Pope et al. (2005) GOODS-N Supermap

~5 years ago SCUBA-2 and CLS

~5 years ago SCUBA-2 and CLS

850um ~5 years ago SCUBA-2 and CLS

450um ~5 years ago SCUBA-2 and CLS

SCUBA HAlf Degree Extragalactic Survey (SHADES)

Coppin et al. (2006) Mortier et al. (2005) SXDF / UDS ~300 hours of SCUBA jiggle mapping

1 degree

SCUBA-2 CLS

Final UDS map close to confusion limited (0.9 mJy/beam) over 1 degree ~500 hours integration

1.0 1.5 2.0 2.5 3.0 1 2 3 4 5 6 SHADES

Coppin et al. (2006)

LESS

Weiss et al. (2009)

σrms (mJy beam−1) Ω(σ < σrms) (degree2)

Geach et al. (2013)

Herschel SPIRE 500um SCUBA-2 450um

S2CLS is a factory for detecting dusty starbursts and AGN at z>1 Excellent ancillary data (e.g. CANDELS) probing stellar emission, redshifts, morphologies ALMA offers HST-matched resolution: directly compare dust and gas to stellar emission on sub-galactic scales Pinpoint counterparts with ~few asec accuracy

Survey paper: Geach et al. (2017)

Maps and catalogue available at: https://doi.org/10.5281/zenodo.57792

CO COSMOS not co complet eted ed during CL CLS… … se see Si Simpson talk later

~3 ~3000 SMGs

1 2 3 4 5 6 7 8 9 10 0.0 0.2 0.4 0.6 0.8 1.0

Completeness S850 (mJy)

UDS Akari−NEP EGS GOODS−N Lockman Hole North COSMOS SSA22

3.5 mJy 4.0 mJy 4.5 mJy 5.0 mJy 5.5 mJy 6.0 mJy 6.5 mJy Sν (mJy beam−1) Sν (mJy beam−1)

5

Sν (mJy beam−1)

10

Sν (mJy beam−1)

15

Sν (mJy beam−1) Sν (mJy beam−1)

0.00

P(Sν)

0.25

P(Sν)

0.50

P(Sν) P(Sν) 7.0 mJy 7.5 mJy 8.0 mJy 8.5 mJy 9.0 mJy

Boost = Recovered / Input flux density Signal−to−noise S850 σinst

3 4 5 6 7 8 9 10 1.00 1.20 1.40 1.60

UDS Akari−NEP EGS GOODS−N Lockman Hole North COSMOS SSA22

Contours at 0.05mJy intervals

Geach et al. (2013)

450um counts and resolving the CIB

GALFORM (Lacey et al. 2015) GALFORM single dish (Cowley et al. 2015) Bethermin et al. (2012) Casey et al. (2013) fit Schechter fit (to 20mJy)

S2CLS combined UDS Akari−NEP EGS GOODS−N Lockman Hole North COSMOS SSA22 Casey et al. (2013) Chen et al. (2013) LESS (Weiss et al. 2009) SHADES (Coppin et al. 2006)

1 10 100 0.1 1 10 100 1000 Sν (mJy) dN dS (degree−2 mJy−1)

GALFORM (Lacey et al. 2015) GALFORM single dish (Cowley et al. 2015) Bethermin et al. (2012) Casey et al. (2013) fit Schechter fit (to 20mJy)

S2CLS combined UDS Akari−NEP EGS GOODS−N Lockman Hole North COSMOS SSA22

1 10 100 0.1 1 10 100 1000 Sν (mJy) N( > Sν) (degree−2)

850um counts with ~3000 sources S850>3.5mJy

Geach et al. (2017)

3 4 5 6 7 8 9 10 −1 1 2 3 Sν (mJy) δ( > Sν) = (ρ − ρ) ρ

UDS Akari−NEP EGS GOODS−N Lockman Hole North COSMOS SSA22

2-sigma over-density in GOODS- N, consistent with previous reports of high-z protocluster in this field (e.g. Daddi et al. 2009, Walter et al. 2012) Field-to-field variance within 50%

• f mean on 15-30 arcminute

scales

Field-to-field variance of number counts

Geach et al. (2017)

ALMA follow-up of S2CLS sources at sub-arcsec resolution

Simpson et al. (2014, 2015)

(and SMA – see Chapman talk)

SCUBA-2 Large eXtragalactic Survey: S2LXS

873 hour large programme to cover 10 square degrees to 2 mJy depth over XMM-LSS and E-COSMOS – HSC deep

• fields. First data taken last week!

Probing bright end of SMG distribution, z>4 population and cross-correlation studies PIs: Geach (UK) & Tamura (JP)

873 hour large programme to cover 10 square degrees to 2 mJy depth over XMM-LSS and E-COSMOS – HSC deep fields Probing bright end of SMG distribution, focused on z>4 population and cross-correlation studies PIs: Geach (UK) & Tamura (JP) S2LXS will be SHADES depth, but over 40x the area

Atacama Large Aperture Submm/mm Telescope

A workshop to discuss the science and technical aspects of AtLAST to be held at ESO-HQ January 17-19 2018 Talk deadline 3 Nov, Registration deadline 8 Dec AtLAST@eso.org

A two-year EU-ALMA study of the scientific merit for – and technical implementation of – an Atacama Large Aperture Submm/mm Telescope (AtLAST) is underway. We now invite the community to join in establishing working groups on science and technology aspects of AtLAST. The science and technology working groups of AtLAST will conclude the study in early 2019 with a public report including recommendations for organizational and financial paths to building an international collaboration.