[OIII] λ 5007Å Emitting Galaxies in the SDSS/3XMMe/WISE Cross-Correlation A. Ruiz, S. Mateos, F.J. Carrera, A. Alonso-Herrero & ARCHES team
ARCHES project ● Astronomical Resource Cross-matching for High Energy Studies (ARCHES) ● Building scientifically-validated spectral energy distributions for XMM-Newton sources. ● Construction of the Enhanced 3XMM catalogue (3XMMe). ● Our goal: explore the possibilities of ARCHES for AGN studies. ● Study of a sample of [OIII] emitting galaxies.
SDSS-DR10/3XMMe/WISE cross-correlation ● Sources in 3XMMe fields classified as “AGN Good” completely observed by SDSS-DR10 ● Cross-match using ARCHES tools ( archesxmatch , by F.X. Pineau ) ○/● 3XMMe fields ● AGN Good fields █ SDSS footprint
SDSS-DR10/3XMMe/WISE cross-correlation SDSS-DR10 ● Three x-matches: (2,555,349 sources) SDSS/3XMMe → P(SX) – 1,650,941 3XMMe (72,497 sources) SDSS/WISE → P(SW) – 8562 8562 SDSS/3XMMe/WISE → P(SXW) – 876,925 ● “True” match: P > 0.9 ● No match: P < 0.1 999,502 WISE All Sky (1,895,348 sources)
SDSS-DR10/3XMMe/WISE cross-correlation ● Three subsamples: – A: match in S, X and W sample A sample A 16,956 16,956 – B: match in S, X not W – C: match in S, W, not X ● 894,887 sources ● MIR data for B: Lang et sample C sample C sample B sample B 870,122 870,122 7,809 7,809 al. 2014 ● X-ray data for C: FLIX upper-limits
Sample of [OIII]emitting galaxies ● Sources with SDSS spectra and: – 0.05 < z < 1.0 – Significant [OIII]λ5007Å emission line – L [OIII] > 10 6.5 L ⊙ ( Heckman et al. 2004 ) ● 1542 sources: – Sample A (SXW): 788 – Sample B (SXW): 4 – Sample C (SXW): 750
Dat a Analysis X-ray data: fitting of X-ray “pseudo-spectra” ● Count-rates of 3XMMe catalogue + adequate – response matrices ~ very low resolution X-ray spectrum – Model: phabs * zphabs * powerlaw → – N H and abs. corrected L X ( Γ =2, fixed) N H = 19±7 cm -2 Optical + IR data: fitting of Spectral Energy Distributions ● ugrizW1W2W3W4 + UKIDSS/2MASS – Templates: – 6 galaxies (SWIRE library, Polleta et al. 2007 ) ● Optical accretion disk ● Rowan-Robinson Dust torus ● 2008 Starburst IR emission ● Optical extinction: Calzetti et al. 2000 –
AGN identification Optical criteria: X-ray criteria: MIR criteria ● Good X-ray fit ● In SDSS-DR12 QSO catalogue ● W1, W2 and W3 → SNR>5 (Pâris et al. 2015) (Pâris et al. 2015) ● In AGN wedge (Mateos+12) ● log L X > 42 erg/s ● Broad Balmer emission lines in the spectra – absorption corrected ● Spectra classified as QSO – at 1σ level (SDSS pipeline) ● If possible, BPT diagram 378 MIR AGN 800 optical AGN 566 X-ray AGN •/× bad BPT ○ /∆ good BPT ∆ AGN ○ Star-forming • / ○ sample A ∆ sample B • AGN
AGN identification ● 935 sources showing AGN features in at least one spectral range ● Sample A: 738 (~94%) ● Sample C: 193 (~26%)
BPT diagram Sample A (SXW) Sample C (SXW) X-ray/MIR X-ray/MIR NOT AGN AGN
AGN MIR wedge
AGN MIR wedge Sample A (SXW) Sample C (SXW) Whole sample
L [OIII] vs L 6 µ m LaMassa+10 AGN SED + AGN [OIII] EW Sample A (SXW) Sample C (SXW) X-r X-ray/M y/MIR IR NOT NOT AGN AGN
L 6 µ m vs L X Mateos+12 Sample A (SXW) Sample C (SXW) X-ra X-ray/MIR /MIR NO NOT AGN
AGN N H distribution Sample A AGN, SXW (MC simulat ions) Sample C AGN, SXW (MC simulations)
AGN L X /L 6 µ m distribution Sample A AGN, SXW (MC simulations) Sample C AGN, SXW (MC simulations)
Summary ● We studied a sample of [OIII] λ 5007Å emitting galaxies selected in a SDSS/3XMMe/WISE cross-correlation (ARCHES). ● We identified the AGN in this sample studying their properties in the optical, X-rays and MIR wavelengths. ● We focused on the differences between an X-ray detected subsample (sample A, SXW) and an X-ray undetected subsample (sample C, SXW). ● Sample A is composed of type I/typeII AGN, bright in X-rays, with mild absorption. Around half of them show a strong stellar emission in the optical and MIR. ● Sample C is composed by a mixture of star-forming galaxies and type II AGN. Lack of X-ray detection consistent with heavy absorption (but no Compton Thick) .
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