Herschel

Seb Oliver
OPTIMISATION WITH
FIR/SUBMM SURVEYS
Exploring the Radio Continuum Universe with SKA Pathfinders
June 2012
Overview
•  Motivation
•  FIR/Sub-mm surveys
•  Herschel Data
•  Herschel Highlights
•  Synergy with Radio Continuum Surveys
MOTIVATION
HerMES Science Motivation
What is the history of Far-IR galaxies?
PACS
PACS
SPIRE
SPIRE
SPIRE
-  How do they assemble and evolve over time?
-  Where have luminous FIR systems gone today?
-  How do FIR galaxies relate to dark matter?
-  What is the role of dust in star formation?
-  What is the connection between dusty star
formation and AGNs?
Herschel Extragalactic Surveys
- Observe at SED peak
- Bolometric far-IR luminosities
- Large and uniform samples
Angular resolution
Survey speed
Constraining Bolometric Luminosity
SCUBA 850µm SPIRE 350µm SPIRE 500µm SPIRE 250µm PACS 160µm Normalised to have same FIR Luminosity PACS 110µm Log νFν z=2.2 Rest-­‐frame wavelength Far Infrared Radio Correlation
& sub-mJy radio counts
Van der Kruit 1971
…
Helou et al. 1985
Condon
1992ARA&A..30..575C
King & Rowan-Robinson 2004
HERSCHEL & SUB-MM
SURVEYS
Herschel Large High-z Surveys
HerMES: Herschel Multi-tiered Extragalactic Survey
•  PACS + SPIRE
•  ~400 sq deg from 20ʹ′×20ʹ′ to 3.6º×3.6º (900 hours) + 12 clusters
•  Bolometric luminosities of galaxies, cosmic SFH
•  Wedding cake to probe range of luminosities and environments
PEP: PACS Evolutionary Probe
•  PACS only
•  2.7 sq deg from 10ʹ′×15ʹ′ to 85ʹ′×85ʹ′ (655 hours) + 10 clusters
•  Resolve CFIRB; LFIR & SFRs
H-ATLAS: Herschel-Astrophysical Terahertz Large Area Survey
•  PACS + SPIRE
•  550 sq deg (600 hours)
•  Large-scale structure, AGN, rare objects
•  Expect ~500,000 detections to z~3, majority at 250 & 350 um
H-GOODS: Herschel-Great Observatories Origins Deep Survey
•  PACS very deep imaging of the GOODS Field (330 hours)
•  SPIRE deep imaging of the GOODS Field (30 hours)
GAMA 9-hr field
Springel et al. (Virgo Consortium)
Oliver et al. 2012 arxiv:1203.2562
SCUBA2
Sub-mm surveys
Scuba2
<z> = 2, Td = 35 K
HERSCHEL DATA
250µm
350µm
500µm
10 arcmin
GOODS-N
Data Quality
1st 15 repeats 2nd 15 repeats 1 arcmin Everything you see is real The power of mul6-­‐wavelength imaging against confusion 500um 350um 250um 160um 100um 24um 3.6um 0.8um 7.5' x 6.5' zoom on the GOODS-­‐North field (10' x 15') 6.5' 7.5 arcmin Herschel Science highlights
STARFORMATION
SPIRE Source Counts
BLAST
P(D)
SPIRE
resolved
BLAST
resolved
SPIRE Source Counts
BLAST
P(D)
SPIRE
P(D)
SPIRE
resolved
BLAST
resolved
Glenn et al. 2010 MNRAS
Resolving the FIR Background
•  Source Counts
250, 350, 500 µm
15%, 10%, 6%
•  P(D)
250, 350, 500 µm
65%, 60%, 45%
•  Stacking TBD
With BLAST:
250, 350, 500 µm
80%, 80%, 85%
SSFRD
Karim et al. 2011ApJ...730...61K
Star-formation main sequence
Karim et al. 2011ApJ...730...61K
Elbaz et al. 2011 A&A 533, A119
FIRC for Herschel
qIR = log10 [(SIR/3.75 × 1012 W m−2)/ (S1.4 GHz/W m−2 Hz−1)]
Ivison et al. 2010 A&A 518 L3
•  30mJy@250mu ~ 60µJy at 1.4Ghz
Herschel Science highlights
CONNECTION WITH AGN
Herschel Science highlights
WEIRD & WONDERFUL
High Redshift Candidates?
500 um peaked sources
Average spectra of sources detected in 4
HerMES fields compared to templates:
Three examples:
250 um 350 um 500 um
*
*Confusion reduced S(500) – fS(250)
Dowell et al. 2011, in preparation
These could be:
z = 1.5, Tdust = 20 K ULIRGs or
z = 5, Tdust = 35 K HLIRGs…
Herschel Science highlights
RELATION TO DARK MATTER
ENVIRONMENT
Large Scale Structure
1-halo
2-halo
Amblard et al. Nature, 2011
•  Spectrum shown after removal of shot noise, cirrus and
correction for the beam window function
•  Clear 1-halo clustering seen
•  Informs minimum halo mass ~3x1011 Msun
Connecting stellar mass and star-formation
rate to dark matter halo mass across 80 per
cent of cosmic time
z
Average SFR
L. Wang, D. Farrah, S.J. Oliver, et al. 2012 MNRAS sub. ArXiv 1203.5828v1.
Present day Halo mass
Herschel Science highlights
COSMOLOGY
Cosmic Magnifica6on K=6.3
K=133
Wang et al. 2011MNRAS.414..596W
Lessons Learned
•  Iterative maximum likelihood Mapping techniques from CMB
•  Dealing with confused maps
-  Work with images, P(D), P(k)
-  Stacking techniques
-  Cross-identification techniques
•  Importance of multi-wavelength data
-  Esp. Spitzer 24 micron data
•  Software effort up front pays off
•  Nothing beats having a good instrument
•  Good communication between instrument/software/scientists
•  Simulations key for science analysis
•  Survey planning, science validation/demonstration, flexibility
SYNERGY WITH RADIO & PATH
FINDER CONTINUUM SURVEYS
FIR/Radio Synergies
•  Bolometric calibration for SFR
•  Radio surveys will continue SFR investigations to lower SFR and
better statistics
•  Radio/FIR photo-z
•  Morphologies for starbursts
•  Radio identifications for interesting FIR/sub-mm sources
•  SFR / AGN connection
e.g. through stacking
SFR Hα
SFR infrared
FIR/sub-mm should give
bolometric calibration of
radio SFR estimators
SFR UV
Comparison of Star
Formation Rate
measures
Cram et al 1999
Star formation rates in the radio
Solar masses per year
E.g. SFR from LOFAR
HerMES level 5
LOFAR Tier 2
LOFAR Tier 3
Radio / FIR photo-z
Carilli and Yun 2000ApJ...530..618C
Carilli, C. L., & Yun, M. S. 1999, ApJ, 513, L13
Compactness
Elbaz et al. 2011 A&A 533, A119
LOFAR & Herschel
Herschel:
LOFAR Tier 3
LOFAR Tier 2
L1
GOODS
South
0.11 □°
LOFAR Tier 1
MIGHTEE Tier 3
L2
0.36 □°
L3
1.25 □°
GOODS
North
Lockman
North
ECDFS
Lockman
East
MIGHTEE Tier 2
EGS
EMU
UDS
e-Merlin
L4
4 □°
L5
30 □°
L6
40 □°
L7
270 □°
COSMOS
CDFS
FLS
ELAISS1
XMMLSS
ELAISN2
UDS
EGS
Lockman
Akari
SEP
VVDS
Bootes
Bootes
ELAISN1
ELAIS-N1
ELAIS-S1
HeLMS / Stripe 82
H-ATLAS North
H-ATLAS South
XMMLSS
Conclusions
•  Herschel & sub-mm surveys are scientific and technical
pathfinder for SKA pathfinders
•  Scientific and technical synergies are strong
•  Important to put pathfinder surveys in Herschel fields
•  Luckily that’s what we’ve done!
EXTRA SLIDES
Star-formation main-sequence
Elbaz et al. 2011 A&A 533, A119
CIRB from stacking 24µm sources
hermes.sussex.ac.uk HERSCHEL MULTI-TIERED EXTRAGALACTIC SURVEY
Seb Oliver: COSMOS meeting 14th June 2011
Bruno Altieri, Alex Amblard, Vinod Arumugam, Robbie Auld, Herve Aussel, Tom Babbedge, Alexandre
Beelen, Matthieu Bethermin, Andrew Blain, Jamie Bock, Alessandro Boselli, Carrie Bridge, Drew
Brisbin, Veronique Buat, Denis Burgarella, Nieves Castro-Rodriguez, Antonio Cava, Pierre Chanial, Ed
Chapin, Scott Chapman, Michele Cirasuolo, Dave Celments, Alex Conley, Luca Conversi, Asantha
Cooray, Darren Dowell, Naomi Dubois, Eli Dwek, Simon Dye, Steve Eales, David Elbaz, Duncan
Farrah, Patrizia Ferrero, Matt Fox, Alberto Franceschini, Walter Gear, Elodie Giovannoli, Jason Glenn,
Eduardo Gonzalez-Solares, Matt Griffin, Mark Halpern, Martin Harwit, Evanthia Hatziminaoglou,
Sebastian Heinis, Peter Hurley, HoSeong Hwang, Edo Ibar, Olivier Ilbert, Kate Isaak, Rob Ivison,
Guilaine Lagache, Louis Levenson, Nanyao Lu, Suzanne Madden, Bruno Maffei, Georgios Magdis,
Gabriele Mainetti, Lucia Marchetti, Gaelen Marsden, Jason Marshall, Angela Mortier, Hien Nguyen,
Brian O’Halloran, Seb Oliver, Alain Omont, Francois Orieux, Mathew Page, Pasquale Panuzzo, Andreas
Papageorgiou, Harsit Patel, Chris Pearson, Ismael Perez-Fournon, Michael Pohlen, Jason Rawlings,
Gwen Raymond, Dimitra Rigopoulou, Laurie Riguccini, Davide Rizzo, Giulia Rodighiero, Isaac
Roseboom, Michael Rowan-Robinson, Miguel Sanchez-Portal, Bernhard Schulz, Douglas Scott, Nick
Seymour, David Shupe, Anthony Smith, Jason Stevens,, Myrto Symeonidis, Markos Trichas, Katherine
Tugwell, Mattia Vaccari, Elisabetta Valiante, Ivan Valtchanov, Joaquin Vieira, Laurent Vigrouz, Lingyu
Wang, Rupert Ward, Don Wiebe, Gillian Wright, Kevin Xu, and Mike Zemcov, + Consultants and
Working Members
Faculty and Researchers, Postdocs, Students
Lensing in Hermes by a Galaxy Group
Bright source found by HerMES: 420 mJy at 250 um
SMA Keck NIRC2 LGS AO
Subaru image
Gavazzi et al. 2011
Lensed Galaxy in Hermes/Lockman
ZSPEC: HERMES J105751.1+573027
z = 2.958 +/- 0.007
Scott et al. 2011
UK-SCUBA
450/850 µm Surveys
Hughes et al.
Hughes et al. 1998 Nature 394 241
1200 µ map of the brightest SCUBA source
HDF850.1 (Downes et al. 1999, A&A 347, 809)
Liverpool
(source possibly identified with obj. 3-593.0 at z=1.75)
3-Dec-2003
See also Scott et al 2002 MNRAS 331, 817 & Fox et al. 2002 MNRAS 331, 839
Dust temperature
distribution
z = 0-­‐2.5 Herschel z = 0 AKARI + IRAS Hwang et al. (2010)
MNRAS 409, 75
ArXiv:1009.1058v1
See also Chapman et
al. (2010) MNRAS 409,
75 & Magdis et al 2010,
409, 22
•  marginal evoluSon of LIR-­‐Tdust •  mildly colder (U)LIRGs by ~2-­‐5 K •  envelope extends to colder SMGs Star formation & AGN
•  In 250/70 vs 70/24 colours the AGN are disSnct from the star forming galaxies. •  In 500/350 vs 350/250 colours, star forming galaxies and AGN are indisSnguishable. Hatziminouglou et al. 2010 SFRD in radio
HerMES Survey Design
Level Are
a
> 75 galaxies per Δlog(L)*Δz = 0.1 bin
Lagache 2003 galaxy model
Cover sufficient area to see large-scale
structure and avoid sample variance
Oliver et al. 2012 arxiv:1203.2562
Outliers
LIR for Starbursts and AGNs
Multi-Wavelength SED Fits
Priors: S24, z, SB/AGN
Elbaz et al. 2010
A&A 518, L29
Cold cirrus component
Rowan-Robinson et al. 2010
1 Repeat 2 Repeats 4 Repeats 8 Repeats SPACE FOR SLIDE SHOWING
15 Repeats 30 Repeats IMAGES OF EITHER A2218 OR
GOODS N AT DIFFERENT DEPTHS
28 arc min Nguyen et al. A&A 518 pp. L5
Herschel SPIRE surveys
Oliver et al. 2012 arxiv:1203.2562
Large Scale Structure
Angular Correlation of Detected Galaxies
Cooray et al. 2010
•  Spatial clustering of (z~2) galaxies compared to halo model
•  Halo needed to host a S250 > 30 mJy FIR galaxy: M = 1012.6 Msolar
•  ~15% appear as satellites in more massive halos M ~ 1013.1 Msolar