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An X-ray/radio sample of Active Galactic Nuclei
Nuria Fonseca Bonilla
Tutor: Stefano Bianchi Matteo Guainazzi


An X-ray/radio sample of Active Galactic Nuclei

Brief introduction Results Conclusions


An X-ray/radio sample of Active Galactic Nuclei

1. What does Active Galactic Nuclei

mean?
The term AGN refers to:
Extreme luminosities (L~1042 ­ 1046 erg s-1) not produced by stars Luminosity comes from a very compact region (nucleus) implies the presence of SMBH The main and more efficient mechanism to produce energy is accretion ACCRETION DISK


An X-ray/radio sample of Active Galactic Nuclei

2. Classification of AGN
radio loud (powerful jets):
e.g: radio galaxies, quasars, blazars...

radio quiet
radio quiet quasars (RQQs)
Veron `06: MABS < -23

Seyfert
Veron `06: MABS > -23


An X-ray/radio sample of Active Galactic Nuclei

3. Unification Model
Geometrical effects are important:
Seyfert 1s
Narrow and broad lines

Seyfert 2s
Only narrow lines

Seyfert 2 Seyfert 2

Seyfert 1 Seyfert 1


An X-ray/radio sample of Active Galactic Nuclei

4. AGN emissions:

Optical/UV band: "big blue bump" Accretion Disk IR band: thermal emission Dust (torus) Radio Jet X-ray Comptonization of disk photons Soft: 0.5-2keV Hard: 2-10keV

Wide spectrum Emission in all bands


An X-ray/radio sample of Active Galactic Nuclei

5. Advantages of a multiband analysis
Each component has a different origin Better knowledge of the properties of an AGN Main goal of this project: DATA CORRELATION X-ray data (XMM Newton) Radio and optical data (catalogues)
Vizier:http://vizier.u-strasbg.fr/viz-bin/VizieR NED:http://nedwww.ipac.caltech.edu/ nedwww.ipac.caltech.edu ADS:http://adswww.harvard.edu/ SIMBAD:http://simbad.u-strasbg.fr/


An X-ray/radio sample of Active Galactic Nuclei

6.Data X-ray:
116 Type 1 AGN targeted by XMM-Newton Luminosities in both bands: hard & soft Main spectral properties (iron line, spectral index...)

Optical:
MABS to distinguish between Quasars and Seyfert

Radio:
Flux in 6cm (5GHz) and 20cm (1.4GHz)


An X-ray/radio sample of Active Galactic Nuclei

(1) Veron 2006 Quasars and Active Galactic Nuclei (2) Kellerman 1989 VLA observations of objects in the Palomar Br ight Quasar Survey (reference in Veron for data, some with upper limit (#) <0.25mJy) (3) Kuhn 2001 A Search for Signatures of Quasar Evolution (reference in Veron for (4) Condon 1998 (5) Gregory 1996

6.Data X-ray:

REFERENCES (RQQ):

116 Type 1 AGN targeted by XMM-Newton data, with upper limit (#)) Luminosities in both bands: hard & soft Main spectral properties (iron line, spectral index...)
REFERENCES (Sy1):

(1) Veron 2006 Quasars and Active Galactic Nuclei

Optical:
M

(2) Kellerman 1989 VLA observations of objects in the Palomar Br ight Quasar Survey ABS (reference in Veron for data, some with upper limit (#) <0.25mJy) (3) Gregory 1991

to distinguish between Quasars and Seyfert

Radio:

REFER NCES(NLSY) Flux in 6cm (5GHz)Eand 20cm (1.4GHz) (1) Veron 2006 Quasars and Active Galactic Nuclei (2) Kellerman 1989 VLA observations of objects in the Palomar Br ight Quasar Survey


An X-ray/radio sample of Active Galactic Nuclei

7. Example of a table of data: NLSY
COORDENATES | NAME | RA J2000 08 42 48 25 37 53 30 27 42 59 18 46 07 13 05 51 45 36 39 34 06 23 41 57 | DEJ2000 | F6CM |RF F20CM |RF|MABS| 33 43 22 24 23 41 59 10 26 01 48 48 42 12 55 09 46 43 19 38 03 31 04 22 06| | 32|0.009 | 07| | 54| | 04|0.007 | 36|0.003 | 53| | 44| | 23|0.001 | 47|0.001 | 47|0.006 | 45|0.038 | 55|0.002 | 26|0.132 | 34|0.001 | 27|0.001 | 10|0.001 | 55|0.0005| 21| | 29| | 44| | 07| | 58| | 56| | | | |-20.9| 1|0.028|1|-21.0| |0.001|1|-25.0| |0.006|1|-24.2| 1|0.020|1|-24.1| 1|0.008|1|-23.4| |0.003|1|-20.3| |0.004|1|-20.2| 1|0.003|1|-23.4| 1|0.003|1|-20.7| 1|0.040|1|-20.1| 1| | |-20.8| 1| | |-24.2| 1|0.331|1|-17.9| 1|0.001|1|-24.5| 1|0.004|1|-23.0| 1|0.002|1|-25.0| 2| | |-25.0| | | |-25.2| |0.026|1|-21.4| |0.004|1|-20.8| | | |-21.7| | | |-26.9| | | |-23.3| 107.172917 -49.551778|1H0707-495 340.663939 29.725364 |AKN564 207.143750 26.368611 |E1346+266 201.330333 -38.41486 |IRAS13224-3809 204.328032 24.384242 |IRAS13349+2438 13.395585 12.693390 |IZW1 37.522704 -8.997943 |MRK1044 21.885635 19.178833 |MRK359 220.531097 35.439701 |MRK478 239.790109 35.029865 |MRK493 184.610456 29.812872 |MRK766 311.586954 -2.812579 |MRK896 31.957764 2.715532 |NAB0205+024 213.311942 -3.207487 |NGC5506 211.317479 25.926369 |PG1402+261 222.786542 27.157500 |PG1448+273 236.376000 48.769194 |PG1543+489 339.032000 13.732028 |PG2233+134 24.982505 6.322593 |PHL1092 158.660829 39.641158 |RE1034+396 46.664875 0.062000 |RXJ0306.6+0003 50.813792 -49.518389 |RXJ0323.2-4931 340.481250 -44.081944|RXJ2241.8-4405 14.333101 -22.383083 |TONS180 |07 |22 |13 |13 |13 |00 |02 |01 |14 |15 |12 |20 |02 |14 |14 |14 |15 |22 |01 |10 |03 |03 |22 |00 41.5|-49 39.3|+29 34.3|+26 19.2|-38 18.8|+24 34.9|+12 05.5|-08 32.5|+19 07.5|+35 09.6|+35 26.5|+29 20.8|-02 49.8|+02 14.8|-03 16.2|+25 08.8|+27 30.2|+48 07.7|+13 55.8|+06 38.6|+39 39.5|+00 15.3|-49 55.3|-44 20.2|-22


An X-ray/radio sample of Active Galactic Nuclei

8. Final results: HIGH ENERGY band [2-10keV]

GOOD CORRELATION: no differences

between objects


An X-ray/radio sample of Active Galactic Nuclei

8. Final results: LOW ENERGY band [0.5-2keV]

GOOD CORRELATION: no differences

between objects objects


An X-ray/radio sample of Active Galactic Nuclei

8. Final results: ratio SOFT/HIGH bands

NLSY (red): higher soft excess than other sources No evidence of correlation with radio


An X-ray/radio sample of Active Galactic Nuclei

9. Further analysis Searching FWHM H in literature to reclassify sources:
Narrow lines < 2000km/s Broad lines > 2000km/s

Analysis in other bands Further analysis with other parameters and correlations


An X-ray/radio sample of Active Galactic Nuclei

10.Conclusions Search in catalogs for data:
MABS to separate Quasars and Seyfert Radio fluxes looking for correlations FWHM to reclassify in NL and BL

Results:
Good correlation between X-ray/radio
Both emissions related with main parameters of AGN (mass, accretion rate...) Not depends on the object

Large soft excess in NLSY