caha, 5 feb 2005xmm-newton surveys xavier barcons

CAHA, 5 Feb 2005 XMM-Newton Surveys

XMM-Newton Surveys

Xavier Barcons


Acknowledgements

• The XMM-Newton Survey Science Centre (SSC), especially Mike Watson, Christian Motch, Francisco Carrera, Axel Schwope and Mat Page among others

• The Lockman Hole team, especially Günther Hasinger and Andy Fabian

• The X-ray Astronomy group at my Institute (IFCA), the only (and best) one in Spain

• The Spanish National Space Programme (project ESP2003-00812)

• The whole XMM-Newton project for support and making things happen, including SOC, SSC, instrument teams, Users Group and more.


Index

• What do X-rays tell us about the Universe?• The XMM-Newton X-ray space observatory• The XMM-Newton serendipitous X-ray

survey• The XMM catalogue• Extragalactic Surveys• Surveying the Galactic Plane• The future of XMM-Newton surveys


Physical processes that produce X-rays

• Plasmas (ionised gases) at temperatures of millions of degrees (bremsstrahlung and line emission)

• Very energetic electrons in strong magnetic fields (synchrotron radiation)

• Inverse Compton scattering on high energy electrons.

• Matter falling towards compact objects or black holes (accretion)

• Electron-positron pair cascades


N132D SNR

Fe line

OVII

OVIII


SNRs and Pulsars

The Crab nebula

Chandra

Pulsar


The magnetic field of isolated neutron stars

First unambiguous detection of cyclotron absorption lines in the X-ray spectrum of an isolated neutron star: direct measurement of the magnetic field strength.

B~8 x 1010 GaussBignami, Caraveo, De Luca & Mereghetti 2003

Cyclotron lines

1E1207.4–5209


The Galactic centre in X-rays


Clusters of galaxies

Coma Sérsic 159-03

CAHA, 5 Feb 2005 XMM-Newton Surveys(Chris Done, Univ of Durham)

The X-ray view of Active The X-ray view of Active Galactic NucleiGalactic Nuclei

C. Done, Durham U


The X-ray spectrum of AGN

Radiation from the accretion disk, reprocessed by a corona of hot electrons

Refection (Fe line and Compton recoil)

Absorption by surrounding material

Soft excess (direct radiation from the accretion disk)


The importance of absorption in AGN: the Cosmic X-ray background

• The spectral energy distribution peaks at ~30 keV

• Unified model: The right mixture of absorbed and unabsorbed AGN produces the spectrum of the Cosmic X-ray background

• Predictions:– The majority of X-rays in

the Universe are produced in absorbed objects

– Many absorbed quasars should be found

Gilli et al 2000


The new X-ray observatories

Chandra (NASA)July 1999

XMM-Newton (ESA)December 1999


How does an X-ray telescope work?


XMM-Newton• Spatially resolved (15“) low-

resolution spectroscopy (E/E~20-50)

• Intermediate resolution dispersive spectrometry (0.03-0.06 Ang, E/E~200-500)

• EPIC: (3) CCD spectroscopic imaging cameras 0.1-12 keV

• (2) Reflection Grating Spectrometers (RGS): 0.05-3 keV

• (1) Optical monitor (OM): Optical/UV imaging and grism spectroscopy.


A new window: Hard X-ray energies

Sensitivity to hard X-rayenergies (up to 12 keV

with XMM-Newton) RosatXMM/Chandra

log NH=

Absorbed sources can be seen!


The XMM-Newton serendipitous sky survey

• Every new XMM-Newton pointing (with EPIC in full window mode) discovers ~30-150 serendipitous X-ray sources.

• About 30,000 new X-ray sources/year, with positional and X-ray spectral information


The XMM-Newton catalogue

• Compiled by the SSC• All EPIC detected sources, flags

and large amount of information• Accessible through XSA, LUX, CDS• 1XMM released April 2003 (30,000

sources)• 2XMM released 2005 (100,000-

150,000 sources)


1XMM: Sky distribution


1XMM: The X-ray population

B1=0.2-0.5 keVB2=0.5-2.0 keVB3=2.0-4.5 keVB4=4.5-7.5 keVB5=7.5-12 keV

HR1=(B2-B1)/(B2+B1)

HR2=(B3-B2)/(B3+B2)

HR3=(B4-B3)/(B4+B3)


1XMM

Hard sources

Soft sources


The Survey Science Centre identification programme

• Core programme (~1000 sources/sample):– High b faint sample (10-15 erg cm-2 s-1) – High b medium sample (10-14 erg cm-2 s-1)– High b bright sample (10-13 erg cm-2 s-1)– Galactic Plane Sample

• Imaging programme (u,g’,r’,i’,Z,H)• Statistical identifications based on X-ray

properties & imaging programme.


dMe Star

QSOz=0.565

Sy 2z=0.238

NGC 4291z=0.0058

QSOz=2.649

Sy 1z=0.330


The XMM-Newton Medium Sensitivity Survey


The XMM-Newton Medium Sensitivity Survey (XMS)

• 25 XMM fields• XID:0.5-4.5 keV• SXID>210-14cgs• Ω=3.5 deg2

• 298 sources• 200 identified (67%)

Sources Number %

BLAGN 150 75

NELGs 23 12

ALG&Clus 6 3

Stars 20 10

BLLac 1 0

TOTAL 200 100

Barcons et al 2002Carrera et al 2005


Identification strategy

• Deep (~23mag) optical/NIR imaging of full EPIC field of view (La Palma, ESO)

• Search for candidate counterparts• Optical spectroscopy (fibre+long slit)

– AXIS (An XMM-Newton International Survey) international programme at La Palma (April 2000- April 2002)

– Calar Alto, 3.5m telescope with MOSCA (2003-2005)

http://www.ifca.unican.es/~xray/AXIS


XMS spectroscopic identifications

Search for candidate counterpartsi’-band sources within either:

5 (statistical) or5 arcsec

95% of the X-ray sources have a potential optical candidatecounterpartIn > 75% of these cases, the candidate counterpart is unique


40

41

42

43

44

45

46

0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

z

log

L (

0.5-

4.5

keV

, erg

/s)

BLAGN noXabs

BLAGN Xabs

NELG noXabs

NELG Xabs

Gal noXabs

Gal Xabs

XMS: Luminosity vs. redshift

NGC4291


XMS: Optical colours

-1

-0.5

0

0.5

1

1.5

2

2.5

-1 -0.5 0 0.5 1 1.5 2

g-r

r-i

BLAGN noXabs

BLAGN Xabs

NELG noXabs

NELG Xabs

Gal noXabs

Gal Xabs

Stars

-1

-0.5

0

0.5

1

1.5

2

2.5

-1 -0.5 0 0.5 1 1.5 2

g-r

r-i

BLAGN noXabs

BLAGN Xabs

NELG noXabs

NELG Xabs

Gal noXabs

Gal Xabs

Stars

UnID noXabs

UnID Xabs

Early-type galaxiesQSOs

NGC4291

• 228 sources have all both g.r, r-i colours: 60 UnID, 168 ID


XMS: fXID/fopt vs. HR2

-5

-4

-3

-2

-1

0

1

2

3

-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4

HR2

log

(fX

/fo

pt)

BLAGN noXabs

BLAGN Xabs

NELG noXabs

NELG Xabs

Gal noXabs

Gal Xabs

Stars-5

-4

-3

-2

-1

0

1

2

3

-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4

HR2

log

(fX

/fo

pt)

BLAGN noXabsBLAGN XabsNELG noXabsNELG XabsGal noXabsGal XabsStarsUnID noXabsUnID Xabs

NGC4291

Star/AGN separati

on


“Empty” sources and EROs

Fiore et al 2003

Most of these sources areExtremely Red Objects

(EROs) with R-K>5


Extremely Red Objects and obscured AGNs

Brusa, Comastriet al (2004)


The deepest XMM-Newton observation in the Lockman Hole

Distant galaxycluster (z=1.2)

Rotating supermassiveBlack Holes

Absorption inAGN


Lockman Hole800 ks XMM-Newton observation

Average line profile calls for BH rotation

Average rest-frame spectra show relativistic Fe-lines

type-1 AGNEW~500eV

Streblyanskaya et al., 2004

type-2 AGNEW~400eV


Elements formed at z>1.3!

Abundance independent of z

Best X-ray spectrum of a z>1 cluster

kT~5 keVXMM 800 ks

Determination of Fe abundance and redshift in a very distant

cluster

Hashimoto et al 2004


Photoelectric absorptionMedium Survey (XMS)Slim(0.5-4.5 keV)~10-14 erg cm-2 s-1

•10% of type 1 AGN are absorbed(with NH<=1022 cm-2) •40% of type 2 AGN are absorbed

Mateos et al (2004)

Deep Survey (Lockman Hole)Slim(0.5-4.5 keV)~10-14 erg cm-2 s-1

•15% (<30% at 3) of type 1 AGN are absorbed (with NH<1022 cm-2) •80% (>50% at 3) of type 2 AGN are absorbed. But 5/28 are unabsorbed

Mateos et al (2005)


Type 1 AGN (moderately) absorbed in X-rays

S 0.5-4.5 keV= 7.2 x 10-14 erg cm-2 s-1

z=0.872 NH=2.81021 cm-2

Broad-Line AGN

L 2-10=3.21044 erg s-1

WHT/ISIS

XMM

XMMU J061515.2+710204


A type 1.9 AGN with no absorption

Barcons, Carrera & Ceballos 2003

H1320+551, z=0.0653Seyfert 1.8/1.9H/H>27Expected absorption: >1022 cm-2

XMM-Newton:Disk + reprocessingAbsorption<1020 cm-2


X-ray/optical mismatches: variability?Simultaneous XMM-Newton and 3.5m/CAHA spectroscopy ofMkn 993; z=0.0155 (Changing type Seyfert)

3.5m/TWINXMM

Optical: Seyfert 1.8Balmer decrement=9(NH~ 5 1021 cm-2)

X-ray: weak absorption (NH~ 7 1020 cm-2)

Optical spectral typeintrinsic to BLR,

not due to absorption


ESO 602-G031 (Sy 1.8)

MRK 702 (Sy 1.9)

UGC 12138 (Sy 1.8)

soft component

soft component soft component

z=0.0356

z=0.0250z=0.0337

No or verylow intrinsicabsorption !!!

More type 1.8-2 AGN with no X-ray absorption

Lehmann et al 04


Type 2 AGN without absorption (Lockman Hole

deep survey)Type 2 AGN(narrow lines only)

z=0.711=1.8NH=0

Mateos et al 2005


Type-2 Radio-Quiet QSOs

AAT/2dF(Mat Page)

NH~5 1022 cm-2

z=2.978 (Ly, CIV, CIII])X-ray flux (2-10 keV) = 8 10-15 erg cm-2 s-1

Intrinsic X-ray luminosity = 4 1044 erg s-1

XMM


Optically dull, X-ray luminous galaxiesz=0.044

LX=1042 erg/s

TNG

Subaru

=1.7NH=2 1023 cm-2

XMM

Severgnini et al (2003)


Optically dull, X-ray luminous galaxies (“Fiore 3”)

R=18, z=0.15Early type galaxy

Flux (2-10 keV)=3 10-14 erg cm-2 s-1

Comastri et al 2002

caha, 5 feb 2005xmm-newton surveys xavier barcons

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