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The LABOCA Survey of the ECDFS – submm properties of NIR-selected
galaxies Thomas R. Greve (MPIA), Axel Weiss, Attila Kovacs, Fabian Walter, Ian
Smail, Peter Kurczynski & the rest of the LESS Team
APEX
LABOCA
Charlottesville, September 2009
E-CDFS: 30’ x 30’ field Ra 03:30h Dec -27:40 deg
Wavelength coverage:X-ray: Chandra, XMMUV: GALEXOpt: MUSYC, HST GEMS/GOODS, COMBO-17IR: SIMPLE (IRAC), FIDEL (MIPS)Radio: VLA 1.4GHz
30’
LABOCA-ECDFS Survey - The Field
HST Chandra
Milky Way HI
E-CDFS
GOODS-south
LABOCA-ECDFS Survey - Instrument
LABOCA:
Wavelength: 870 µmBandwidth: 60 GHz
Resolution: 19.2’’FoV: 10.4’
Pixels: ~250Sensitivity: 50 mJy √s
Map rms after 280hrs on source: =1.2 mJy/b (beam smoothed)
Same area but ~2 lower noise levelthan largest SCUBA survey (SHADES)
LABOCA-ECDFS Survey - Noise Properties
rms map
ECDFS
Shades
1.1 mJy/b
1.2 mJy/b
Weiss et al. (2010)
LABOCA-ECDFS Survey – S/N map
What’s the nature of the submm faint (<0.5mJy) galaxies?
Reverse strategy: select high-z galaxies populations at other wavelengths (than submm) and search for a statistical signal
Infer average IR-luminosities, SFRs, EBL-contribution and SF-laws as a function of z and stellar mass
The zoo of near-IR selected galaxies
Why the near-IR?
• near-IR selection is relatively immune to dust and age effects on the stellar population (unlike UV/optical)
• near-IR selection is essentially a stellar mass selection
• the near-IR is able to probe the low mass-end of galaxies compared to submm and radio surveys
• recent advent of large-format near-IR cameras
Near-IR surveys have revealed populations of star forming galaxies and very old, red galaxies at 1 < z < 3, e.g. ERO, DRG, BzK Galaxies
The Multi-wavelength Yale-Chile Surveyhttp://www.astro.yale.edu/MUSYC/
• UBVRIzJHK imaging covering the entire ECDF-S (30’x30’)
• 5sigma AB limiting magnitudes:
U (26.8)B (27.0)V (26.6)R (26.4)I (24.7)z (24.0)J (23.0)H (21.6)K (22.3)
• Ready-to-go catalogues available on-line
K-selected sample: Kvega ≤ 20
We also extracted BzK, ERO & DRG samples (selected down to Kvega ≤ 20)
BzK Galaxies (star forming and passive) - selection
sBzK(z-K)AB - (B-z)AB ≥ -0.2
pBzK(z-K)AB - (B-z)AB < -0.2
STARS
EROs and DRGs - selection
STARS
ERO(R-K)AB > 3.35
DRG(J-K)AB > 1.32
Final Catalogues
STARS
ERO(R-K)AB > 3.35
DRG(J-K)AB > 1.32
Kvega 20 : 8266
sBzK : 744
pBzK : 149
ERO : 1253
DRG : 737
Photometric Redshifts
Phot-z’z are derived using EAZY code (Brammer, van Dokkum & Coppi 2008)
Applied to the UBVRIzJHK MUSYC photometry
σ(Δz) = 0.037 z < 1.5
σ(Δz) = 0.079 z > 1.5
Stellar massesDerived using Hyper-z on the UBVRIJHK (MUSYC) + IRAC (SIMPLE) photometry
Bruzual & Charlot +03: SPP, Exp (300) and Constant SF histories. Calzetti dust (Av = 0-3)
Use rest-frame H-band luminosity since M/LH is less sensitive to AGN and TP-AGB stars
Submm Stacking of K-selected galaxies • Remove robust submm sources in map
• Go to positions of near-IR selected galaxies in the submm map and read of the signal and noise
• Weighted mean stacked flux and noise
• Deblending
Submm Stacking of K-selected galaxies
Full stacks…
3x
5x
Average 870μm flux vs. redshift for Kvega ≥ 20 selected galaxies
Submm Stacking of K-selected galaxies
• IR luminosities:sBzK: (2-6)x1011L
pBzK: (1-3)x1011L
ERO: (1-4)x1011L
DRG: (1-4)x1011L
•Star formation rates:sBzK: (30-100)Myr-1
pBzK: (10-50)Myr-1
ERO: (20-60)Myr-1
DRG: (20-60)Myr-1
• Background resolved:Kvega < 20: 15%sBzK/ERO/DRG: ~4% (each)
Submm Stacking of K-selected galaxies
As a function of 24μm flux (using the FIDEL MIPS catalogue: > 27μJy 5-σ)
• 24μm detected sources have 5x higher average 870μm flux than 24μm non-detections
• Linear correlation (S24μm < 350μJy):
S870μm = 4.5x10-3 x S24μm
• “Flattening” at S24μm > 350μJy
• 24μm traces starformation, but significant contribution from AGN for very bright 24μm systems (although selection function is non-trivial).
Stacking across the BzK-diagram
Refining the sBzK/pBzK selection criteria?
SSFR vs. z and Mstar – evidence of downsizing?
Total SFR (UV+FIR)
Summary • The largest submm stacking analysis of K-selected galaxies, allowing us to probe 7x deeper than typical blank field submm surveys
• Significant submm signals for sBzK, ERO and DRG galaxies. pBzKs are not detected (<0.3mJy). Typically: LIR = (2-6)x1011L and SFR = (60-100)M yr-1
• We find a strong increase in the submm-flux (star formation rate) of near-IR selected galaxies at z > 1.5. This means the dust-enshrouded star formation rate was higher at earlier cosmic epochs
• We find a linear 870μm-24μm correlation for S24μm < 350μJy, suggesting that 24μm is a good tracer of starformation for such systems. For brighter 24μm systems the relation flattens, consistent with an AGN contribution to the 24μm flux
• Tentative evidence of SSFR-evolution with redshift. Also for downsizing, meaning less massive galaxies have higher SSFRs. This is the first time this kind of work has been done using the submm!
• See also poster by Peter Kurczynski