THE NEP-DEEP SURVEY- CURRENT STATUS -

Toshinobu Takagi (ISAS/JAXA - AKARI fellow)

ContentsOverview of the NEP-Deep surveyImage quality

Band-merged cataloguesAll-band-detected sourcesMIR-detected sources

Photometric redshifts

Ancillary data

The NEP Survey★ Deep : 0.38 deg2 (224 pointing)★ Wide : 5.8 deg2 (450 pointing)

NEP-Wide

NEP-Deep

1 deg

NIR: 2, 3, 4 μmMIR-S: 7, 9, 11μm MIR-L: 15, 18, 24μm

★ In all IRC bands

NEP-Deep

AKARI/IRC 2,3,4µm colour image

Subaru/S-cam fieldDeep B,V,R,i’,z’KP2.1m/FLMN J,KsKeck/DEIMOS spec.

More data from GALEX, CFHT (u*griz, YJKs), AKARI/mid-IR spectroscopy,AKARI/FIR survey, WSRT(1.4GHz) GMRT(610MHz)

IRC Images and Weights

Integration time (MIR): 1000 - 1500 sec

AstrometryN3 S7 L15

versus 2MASS

Wada et al. (2008)

NEP Deep summary

Wada et al. (2008)

4.27.54647

210

9.67.55.4

28.9SWIRE23.519.7

Polletta et al. (2007)

Example of Spitzer SEDs

AKARI SEDs

CataloguesAll-band-detected source catalogueSources are detected in a MIR-S combined image.IRC sources with the angular separation of <3 arcsec are regarded as the same source. Optical ID is done with the nearest neighbor finding.All optical-ID have been eye-ball checked.

Sources detected in all 9 IRC bands (1100)

Found in Subaru/S-cam field (630)

Excluding ambiguous optical identification (568)

With spectroscopic data (113)

AKARI/IRCN2, N3, N4 S7, S9W, S11 L15, L18W, L24

IRC colour images

PAH-selected galaxies

IRC colour imagesSubaru/BRz’ N2 N3 N4 S7 S9W S11 L15 L18W L24

PAH-selected galaxies

Starburst SED model

PAH-selected galaxies★ Selection: flux ratio (in Jy) F(11)/F(7)>8 or F(15)/F(9)>8★ Much redder than AGN with the steepest power-law (→ 15/9μm ratio = 3.6)

Takagi et al. (2010, submitted)F(11)/F(7)

Specific SFRSWIRE template

SED fitting examplePAH-selected galaxies at z~0.5

Good fit for 50% of PAH-selected galaxies

Bad SED fits: example

Bad SED fits: example

Photo-z performanceData: all-band-detected sourcesBVRiz (Subaru), JK(KPNO2m), AKARI IRC 9 bands

Code: Takagi original (Takagi et al. 2008)

Luminosity and MassStarburst (good fit) sample

ULIRGs>3x1010M⦿

More complete catalogue

MIR-S and -L combined catalogue Sources detected in MIR-S or MIR-L images.Source detection was made with MIR-S combined image and also with MIR-L combined image.Two catalogues are concatenated. If source separation is less than 3”, they are regarded as duplication, resulting 10313 sources.Optical ID has been done with Likelihood Ratio methodBased on the probability distributions derived from all-band-detected sources. Only for S-cam sources

Goto et al. (2010) used this catalogue to derive IR luminosity functions. Band merging with other bands has been done with nearest neighbor.

Photo-z performance

Goto et al. (2010)

Data: FUV, NUV(GALEX), u(CFHT), BVRiz (Subaru), JK(KPNO2m)

Code: LePhare (Ilbert et al. 2006)

8μm Luminosity Func.

Goto et al. (2010)

Summary of data• Imagingsurveywith9near-andmid-IRbandsat2-24micron

• NEP-Deep0.38deg2~2000-2500secexposuresperfilterperfield• NEP-Wide5.8deg2~300secexposuresperfilterperfield

• Multi-wavelengthfollow-up• NEP-Deep

• Subaru/S-cam(BVRiz+NB711)Wadaetal.• KPNO2m(JKs)Imaietal.(2007)• CFHT(WIRcam)Goto,Ohyamaetal.• GALEX(FUV,NUV)Malkanetal.• CFHT/Megacamu-bandSerjeantetal.• GMRT(610MHz,40’φ)Serjeantetal.• WSRT(1.4GHz,1deg2)Whiteetal.• Far-IRimagingsurveywithFIS(65,90,140,160μm)Oyabuetal.

• Subaru/FOCASspectroscopyfor574µm-selectedsourcesTakagietal.• KeckII/DEIMOSspectroscopyfor420sources(242sourcesareMIR-selected)Takagietal.• HectospecspectroscopyforselectedtargetsImetal.• GTCspectroscopyacceptedMiyajietal.