Spectra for a million* radio galaxies
* nearly
Majority of slide content stolen from Dan Smith [U.Hertfordshire] - P.I. of WEAVE-LOFAR
Resolution
Selection / Statistics
Depth
Resolution
Depth
Selection / Statistics
Dutch stations: only these used for large area survey
Core 'superterp'
Core 'superterp'
HBA : 120 - 240 MHz
LBA : 30 - 80 MHz
Core 'superterp'
LBA : 30 - 80 MHz
HBA : 120 - 240 MHz
Tier-1 : will cover whole northern hemisphere
(0.1 mJy RMS at 150 MHz)
Tier-2 : ~100s of sq.deg to faint flux limits (25 μJy RMS @ 150 MHz)
Tier-3 : ~10s of sq.deg to sensitivities > the deepest existing imaging
(6 μJy @ 150 MHz)
Details: Röttgering et al. 2011
Relative to other radio surveys
In physical terms...
In physical terms...
Tier 1
Tier 2
Tier 3
Tier 3
Tier 2
Tier 1
In physical terms...
Tier 1
Tier 2
Tier 3
Tier 3
Tier 2
Tier 1
Evolution in FIR-radio correlation?
Good Ionosphere
Bad Ionosphere
Credit: Ger de Bruyn
http://www.astron.nl/dailyimage/index.html?main.php?date=20140307
Credit: Tim Shimwell
Credit: Tim Shimwell
(W. Williams+ 2016)
8 Hrs of observations at 150 MHz
(now ~60 observed)
~19 sq.deg
RMS ~120-150 uJy/beam
~6" beam
http://www.ing.iac.es/weave/science.html
PI: Dan Smith, U. of Hertfordshire
“There’s nothing as useless as a radio source”
Jim Condon, 2013
Many LOFAR sources are precisely the populations where photo-z's break down,
e.g. ...
Spectra required to separate SF and RQ-AGN, distinguish accretion modes (high-/low-excitation) etc
and
Spectroscopic follow-up of many LOFAR sources
Resolved spectroscopy of protocluster fields (Ly-alpha/OII emitters around radio AGN)
The MOS surveys have three primary science cases:
Simulations indicate that redshift success rates approach 100% at z < 1
WIDE Tier
All sources with S(150) > 10mJy over 10,000 sq.deg
Highlights:
Based on SKA Simulated Skies (Wilman et al. 2008, 2010)
MID Tier
~250k+ spectra over ~1250 sq.deg
(HETDEX Spring field/H-ATLAS NGP/COSMOS/XMM-LSS)
Highlights:
Based on SKA Simulated Skies (Wilman et al. 2008, 2010)
DEEP Tier
~360k+ spectra over ~70-200 sq.deg
(e.g. Elais N1 / Bootes / Lockman Hole )
Highlights:
Based on SKA Simulated Skies (Wilman et al. 2008, 2010)
The LIFU survey aims to study
The mIFU survey aims to study:
IFU survey aimed at filling poor weather (/bright time) queue
WEAVE-LOFAR IFUs are set-apart by:
IFU survey aimed at filling poor weather (/bright time) queue
Resolution
Depth
Selection / Statistics
~1 million spectra
Unique selection criteria - low frequency radio
Emission lines only
S******g required for detailed spectral properties
R = 5000 (370-960nm)
1 hr exposures - individual spectra only targetting emission line detections
Up to 4x 1 hr exposures on 'unsuccessful' redshifts in DEEP
St****ng
Environment
Mass
AGN activity
Redshift
?