detecting faint submm galaxies using radio lensing the case of the cluster ms0451
DESCRIPTION
Detecting faint submm galaxies using RADIO lensing the case of the cluster MS0451. Dr . Léon Koopmans ( Kapteyn Institute) Prof. Mike Garrett (ASTRON) Dr. Olaf Wucknitz ( AIfA Bonn) . Alicia Berciano Alba ( Kapteyn Institute). OZ Lens 2008, Sydney (Australia) . - PowerPoint PPT PresentationTRANSCRIPT
DETECTING FAINT SUBMM GALAXIES
USING RADIO LENSING
THE CASE OF THE CLUSTER MS0451
Dr. Léon Koopmans (Kapteyn Institute)Prof. Mike Garrett (ASTRON)
Dr. Olaf Wucknitz ( AIfA Bonn)
OZ Lens 2008, Sydney (Australia)
Alicia Berciano Alba (Kapteyn Institute)
The relevance of dust obscured galaxies
Optical/UV lightIR/submm
dust re-radiated light
~ 50% of the total radiation in the
universe
Critically important to understand galaxy
formation and evolution
dust obscured galaxies
Starburst galaxy SED
dust re-radiated
Submm-galaxies in a nutshell SMGs = dusty, FIR luminous starburst galaxies at high redshift Discovered with SCUBA (JCMT) at 850 mm (Smail, Ivison & Blain 1997)
Bright SMGs(what we can see)
Faint SMGs(the unknown territories)
2 mJy SCUBA’s confussion limit
at 850 mm
Properties of bright SMGs:• Median redshift ~ 2.3• LFIR > 1012 Lsun
ULIRGs • SFR ~103 Msun/yr• Gas-rich mergers• Dust temperature ~
35K• Mgas ~ 1010 – 1011 Msun
Bulk of the submm background
energy at 850 mm(Knudsen , van der Werf & Kneib 2007)
My lab rat : MS0451.6 - 0305
Once upon a time … Borys et al. 2004
Data: Optical : HST F702W, F775W, F850LP NIR (circles) : CFHT JHK’- band Submm (contours): SCUBA 850 mm
Source plane
ERO B
ERO CLBG
~ 10 Kpc
Image plane
Redshifts: LBG ARC1 : z = 2.911 (VLT spectroscopy) EROs* B,C : z = 2.85 (lens model)
*Extremely Red Objects
MERGER!!!
Radio interferometry to the rescue
FIR
Submm
dust re-processed UV radiation from massive stars
synchrotron emmision from electrons generated by SN
Radio
FIR (submm)Massive star
formation
Radio interferometry High resolution “version” of the submm map
High-z starburst:Observed in submm = emitted in FIR
Radio observations :
VLA 1.4GHz (20 cm)
B-array (Berciano Alba et al. 2007)
2 x 4 hours (9th and 10th June 2002)Project ID AN109, PI: NakanishiResolution: 6.34” x 4.87” pa= 7.73
A-array2 x 6 hours (5th and 10th Feb 2006)Resolution: 2.07” x 1.58” pa= -1.19
Data reduction: AIPS + ParselTongue
A+B array naturaly weighted 1.4GHz map
Resolution = 2.78 x 2.18 arcsecs pa=-0.21 rms noise = 10.16 mJy/beam
Grey scale: 3 x noiseContours: 4, 5, 6, 8 and 10 x noise
CR1
CR2
Radio detections located withing the submm emission
4 detections: RJ, E1, E2, E32 tentative detections: C1, C2
SNR ~ 6
SNR ~ 4.5
SNR ~ 4.6SNR ~ 6
SNR ~ 11
SNR ~ 5
(flux ~ 34 mJy)
(flux ~ 23 mJy)
(flux ~ 28 mJy) (flux ~ 42 mJy)
(flux ~ 170 mJy)
(flux ~ 52 mJy)
CR1
CR2
Multi-wavelenght counterparts of the radio detections
AlignmentRadio and NIR map aligned respect to the HST map Radio: 13 sources, rms distance = 0.29” NIR: 93 sources, rms distance = 0.06”
Data Optical: HST ACS F814W ( Moran et al 2007 ) NIR: Subaru CISCO K’-band ( Takata et al 2003 )
Positional Errors Radio: FWHM / (2*SNR) between 0.1” and 0.3” NIR: 0.2” (fitting error for the standard stars used for the astrometry)
White contours: 20cm radio emissionBlue squares: NIR sources Yellow squares: optical arcs produced by a LBG
zphoto = 0.45
Source plane
ERO B
ERO CLBG
~ 10 Kpc
MERGER!!!
Extended source: ~ 3 beams (~ 6”) Peak not consistent with any optical counterpart mayor axis aligned with a posible cluster member
zphoto = 0.4
AGN + radio jet
Not associated with the lensed submm
emission!!!
Radio vs submm emission
Radio contours = 3,4,5,6 and 7 x 30 mJy/beam
CONCLUSIONS ON MS0451 (so far…)
The brightest radio detection (RJ) is not related with the lensed submm emission (probably an AGN jet)
The other radio detections (E1,E2,E3,CR1,CR2) are counterparts of the submm emission
2 radio detections (E1,E2) confirm that ERO B is associated with the submm emission
2 tentative radio detections (CR1,CR2) support the merger hypothesis
THE FUTURE The coming years will see a revolution in
radio / mm interferometric observations: EVLA, eMERLIN, ALMA, SKA, LOFAR…
Window to study high redshift dust obscured universe unnaccesible in optical
Time to think about robust multiwavelenght source reconstruction