Florencia Jiménez Luján Trainee in 2004 A Primordial Quasar. Drawing Credit: Wolfram Freudling et al. (STECF), ESO, ESA, NASA Chris R. Benn (ING) J. Ignacio González Serrano (IFCA) Florencia Jiménez Luján Trainee in 2004 Instituto de Física de Cantabria (IFCA: CSIC – UC, Santander, Spain) Dpto. de Física Moderna (Universidad de Cantabria, Santander, Spain) Isaac Newton Group of Telescopes (ING, La Palma, Spain) 2010 ESAC Trainee Summer Alumni Meeting

Florencia Jiménez Luján 1. Introduction 2. Sample selection 3. Observations and data reduction 4. Physical parameters of the absorbers (C, τ, U, ne, Nion, NH, R, Ėk) an example: SDSS J0217-0854 5. Discussion and conclusions 6. Future work ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján extremely powerful, compact (point-like source in the optical range) and variable source AGN (Active Galactic Nuclei) QUASAR/QSO (QUASi-stellAR radio source / Quasi-Stellar Object): BAL (Broad Absorption Line) quasars (~10 – 20 %) present absorption troughs in the blue wings of ionised UV resonance emission lines (e.g. CIV, SiIV, NV). ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján extremely powerful, compact (point-like source in the optical range) and variable source AGN (Active Galactic Nuclei) QUASAR/QSO (QUASi-stellAR radio source / Quasi-Stellar Object): BAL (Broad Absorption Line) quasars (~10 – 20 %) present absorption troughs in the blue wings of ionised UV resonance emission lines. High velocity outflows of ionised gas originated near the centre. Distances and kinetic luminosities estimates: properties and evolution of the AGN, possible related to AGN feedback mechanisms (e.g. formation and evolution of the supermassive black holes and their host galaxies, enrichment of the intergalactic medium and inhibition of cooling flows). ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

(Active Galactic Nuclei) Urry & Padovani, 1995 Unification of AGN (Active Galactic Nuclei) QSO (Quasi-Stellar Object, or quasar, QUASi-stellAR radio source) in the center of each AGN: black hole surrounded by an accretion disk moving clouds: BLR (fast) & NLR (slow) classification: orientation scenario vs. evolutionary scenario (both???) know the properties & composition of the medium (BLR) (NLR) ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

(Active Galactic Nuclei) Elvis, 2000 BAL NAL No absorbers Unification of AGN (Active Galactic Nuclei) QSO (Quasi-Stellar Object, or quasar, QUASi-stellAR radio source) in the center of each AGN: black hole surrounded by an accretion disk moving clouds: BLR (fast) & NLR (slow) classification: orientation scenario vs. evolutionary scenario (both???) know the properties & composition of the medium ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Montenegro-Montes et al., 2008 Unification of AGN (Active Galactic Nuclei) QSO (Quasi-Stellar Object, or quasar, QUASi-stellAR radio source) in the center of each AGN: black hole surrounded by an accretion disk moving clouds: BLR (fast) & NLR (slow) classification: orientation scenario vs. evolutionary scenario (both???) know the properties & composition of the medium BALQSO have convex radio spectra (typical of CSS/GPS “young” radio sources) CSS: Compact Steep Spectrum; GPS: Gigahertz Peaked Spectrum ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján . redshift: 2.5 ≤ z ≤ 4.2, so that the prominent NV, SiIV and CIV doublets fall within the range of SDSS (4000−9000 Å) magnitude: r ≤ 19 (to allow spectra with good S:N to be obtained in a reasonable time) likely, on the basis of visual inspection of the low-resolution SDSS spectra to show velocity-resolved (i.e. probrably intrinsic), unsaturated, unblended doublets from the above ions. SDSS (Sloan Digital Sky Survey) DR4 (Data Release 4) ~ 200 sources ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján 0217-0854 2MASS (2 Micron All Sky Survey): J = 16.884 H = 15.639 K = 15.104 BALnicity Index BI = 39 ± 17 (Weymann et al. 1991) Absorption Index AI = 3360 ± 90 (Hall et al. 2002) z = 2.5712 r = 18.21 FIRST: 5.6 mJy ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján Medium resolution observations with WHT + ISIS (R ~ 7000) (William (Intermediate dispersion Roque de Los Muchachos Observatory Herschel Spectrograph and La Palma (Spain) Telescope) Imaging System) Reduction with IRAF (Image Reduction and Analysis Facilities): bias subtraction, flat fielding, cosmic-ray removal and wavelength calibration. ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

homogeneous partial covering Ib=1-C(1-e-τ) Ir=1-C(1-e-τ/2) τ: optical depth τ ≥ 0 C: covering factor 0 ≤ C ≤ 1 homogeneous partial covering A: areas ratio 0.5 < A ≤ 1 Ib Ir Wavelength (Å) Flux (arbitrary units) ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

U: Ionisation parameter NH: Total hydrogen column density C, τ, Nion Nion: Column density U: Ionisation parameter NH: Total hydrogen column density ionisation parameter, luminosity & electron density N(v) = 3.77 x 1014f -1 λ-1 τ(v), Savage & Sembach 1991 Hamann 1997 oscillator strength ionisation fractions U, NH estimate of the distance (R) from the absorber to the quasar nucleus and the kinetic luminosity (Ėk) Hamann et al. 2001 : spectral index (SDSS) nH ~ ne: electron density λLL = 912 Å λR = 6500 Å SR: Observed flux in the R band (from magnitude r, SDSS) DL: Luminosity distance (calculator, Wright 2006) ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján BAL: z ~ 2.562 – z ~ 2.534 absorber (a) ~ -860 km/s ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján BAL: z ~ 2.562 – z ~ 2.534 absorber (a) ~ -860 km/s N(CII*)/N(CII) = 1.30 (in cm-2) log ne = 2.1 ± 0.2 (in cm-2) absorber (b) ~ -2100 km/s log ne = 1.7 ± 0.2 (in cm-2) ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján Mini-BAL: z ~ 2.454 (i) log ne = 9.5 – 13 (in cm-2) (BLR) (ii) log ne = 2.5 – 4.5 (in cm-2) (NLR) absorber (d) ~ -10030 km/s ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján Not energetic enough to significantly contribute to AGN feeback processes (Ėk ≤ 0.003 % Lbol). Distances between 0.15 pc and 30 kpc, depending on the assumed values of electron density. Small electron density (BAL), possible related to low energetic outflows. Results independent on the model (~ one order of magnitude). ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Florencia Jiménez Luján Extend the analysis to the rest of our observed quasars (in progress). Search for variability both in the continuum and the absorption lines (in progress). Search for line-locking evidences: radiative pressure (in the near future). a blue component of the doublet of an absorber lies just at the expected position of the red component of the doublet of another absorber High resolution optical observations: excited/ground level lines: electron density estimates (in progress). Properties in other ranges (radio: in progress). ESAC Trainee Summer Alumni Meeting, July 2nd 2010 Florencia Jiménez Luján

Thank you! A Primordial Quasar. Drawing Credit: Wolfram Freudling et al. (STECF), ESO, ESA, NASA