Post on 22-Jul-2020
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.