ARCHES project Astronomical Resource Cross-matching for High Energy - - PowerPoint PPT Presentation

[OIII]λ5007Å 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

• Three x-matches:

–

SDSS/3XMMe → P(SX)

–

SDSS/WISE → P(SW)

–

SDSS/3XMMe/WISE → P(SXW)

• “True” match: P > 0.9
• No match: P < 0.1

SDSS-DR10

(2,555,349 sources)

3XMMe

(72,497 sources)

WISE All Sky

(1,895,348 sources) 1,650,941 876,925 999,502 8562 8562

SDSS-DR10/3XMMe/WISE cross-correlation

• Three subsamples:

– A: match in S, X and W – B: match in S, X not W – C: match in S, W, not X

• 894,887 sources
• MIR data for B: Lang et
• al. 2014
• X-ray data for C: FLIX

upper-limits

sample A sample A 16,956 16,956 sample B sample B 7,809 7,809 sample C sample C 870,122 870,122

Sample of [OIII]emitting galaxies

• Sources with SDSS

spectra and:

– 0.05 < z < 1.0 – Significant [OIII]λ5007Å

emission line

– L[OIII] > 106.5 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 → NH and abs. corrected LX (Γ=2, fixed)

• Optical + IR data: fitting of Spectral Energy Distributions

–

ugrizW1W2W3W4 + UKIDSS/2MASS

–

Templates:

• 6 galaxies (SWIRE library, Polleta et al. 2007)
• Optical accretion disk
• Dust torus
• Starburst IR emission

–

Optical extinction: Calzetti et al. 2000

Rowan-Robinson 2008 NH = 19±7 cm-2

AGN identification

Optical criteria:

• In SDSS-DR12 QSO catalogue

(Pâris et al. 2015) (Pâris et al. 2015)

• Broad Balmer emission lines

in the spectra

• Spectra classified as QSO

(SDSS pipeline)

• If possible, BPT diagram

800 optical AGN X-ray criteria:

• Good X-ray fit
• log LX > 42 erg/s

– absorption corrected – at 1σ level

566 X-ray AGN MIR criteria

• W1, W2 and W3 → SNR>5
• In AGN wedge (Mateos+12)

378 MIR 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 L6µm

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

L6µm vs LX

Mateos+12

Sample A (SXW) Sample C (SXW) X-ra X-ray/MIR /MIR NO NOT AGN

AGN NH distribution

Sample A AGN, SXW (MC simulat ions) Sample C AGN, SXW (MC simulations)

AGN LX/L6µm distribution

Sample A AGN, SXW (MC simulations) Sample C AGN, SXW (MC simulations)

Summary

• We studied a sample of [OIII]λ5007Å 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
• ptical 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) .