Dynamic GALACTIC Cores.


74 views
Uploaded on:
Description
Dynamic GALACTIC Cores Optical ghostly grouping and Radiance Capacity Presentation and a few provisos Sy1/QSO/quasar NLRG/QSO2/Sy2 RL QSO/RQ QSO Point-like/developed
Transcripts
Slide 1

Dynamic GALACTIC NUCLEI Optical ghostly characterization and Luminosity Function

Slide 2

Introduction and a few provisos Sy1/QSO/quasar NLRG/QSO2/Sy2 RL QSO/RQ QSO Point-like/augmented ” Active galactic cores (AGN) are a class of universes where a huge portion of the vitality yield, rising up out of their focuses, is not created by the ordinary cosmic system parts : stars, dust and interstellar gas. This vitality can be discharged over the entire electromagnetic range, from radio waves to gamma rays” Reducing the AGN zoo however much as could reasonably be expected ! Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 3

The UV/optical/NIR range Power-law : radiated by an exceptionally reduced non-warm source (power law) Big Blue Bump : this segment conceivably originates from the BH gradual addition plate (dark body) Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 4

The UV/optical AGN range Power-law Big Blue Bump Small Blue Bump : FeII+Balmer Continuum Broad emanation lines : FWHM > 1500 Km/s Narrow discharge lines : FWHM < 900 Km/s The outflow lines portray the AGN spectra: they are delivered in two separate districts, a subarcsec Broad Line Region (BLR) near the focal motor, and a more broadened Narrow Line Region (NLR). Universe Starlight : generally overpowered by the AGN non-warm continuum and rising in the red piece of the range Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 5

The UV/optical outflow line range Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 6

What we gain from the AGN UV/optical spectra Redshift Classification (optical): Type 1/Type 2 AGN Unification: confirmations Physical condition of the transmitting line gas AGN/StB detachment: Diagnostic Diagrams Unconventional AGNs Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 7

Redshift Discovery of the genuine way of quasar Cosmological Distance Absolute physical amounts ( L,M,size ) Only the optical range ( in some cases UV, close IR ) gives z Easy approach to gauge z Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 8

In 1963 Schmidt recognizes profoundly redshifted Balmer lines in 3C273’s range z = 0.158 (v r = 47500 km/s) Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 9

Redshift Discovery of the genuine way of quasar Cosmological Distance Absolute physical amounts ( L,M,size ) Only the optical range ( here and there UV, close IR ) gives z Easy approach to quantify z Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 10

AGN emanation line spectra Type 1 AGN are those with exceptionally expansive optical/UV allowed discharge lines, with FWHM ~1500-15000 km/s, while the prohibited lines, as [O II ] 3727, [O III ] 4959/5007 , [N II ] 6548/6583 , commonly have FWHM s of request of 500-1000 km/s. Sort 2 AGN have allowed and prohibited lines with give or take the same FWHM , like the FWHMs of the taboo lines in Type 1 objects. The prohibited lines, while smaller than the allowed ones, are normally more extensive than the discharge lines in most starburst systems. Optical Type 1 Optical Type 2 Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 11

AGN Unification: the “standard model” Components: Accretion Disk: r ~ 10 − 3 pc n ~ 10 15 cm −3 v ~ 0.3c Broad Line Region: r ~ 0.01−0.1 pc n ~ 10 cm −3 v ~ few x 10 3 km s −1 Dusty Torus: r ~ 1−100 pc n ~ 10 3 − 10 6 cm −3 Narrow Line Region: r ~ 100 −1000 pc n ~ 10 2 −10 4 cm −3 v ~ few x 10 2 km s −1 Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 12

AGN Unification: the worldview “... A great part of the mixed bag in AGN sorts is only the consequence of differing introduction with respect to the observable pathway. [...] We can characterize an amazing theory in which there are just two fundamental AGN sorts: the radio tranquil and radio loud.” (Antonucci 1993) XBONG Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 13

Spectral order (em.lines) Type 1 Type 2 Starforming cosmic systems Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 14

Spectral grouping (em.lines) Type 1 Type 2 Starforming worlds How we can segregate the tight line objects? Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 15

Spectral grouping (em.lines) SDSS DIAGNOSTIC DIAGRAM Sy 1 cosmic systems Sy 2 universes Starforming worlds Composite cosmic systems Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 16

Diagnostic Diagrams SDSS Sy2/StB hypothetical partition Kewley et al. (1991) Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 17

Diagnostic Diagrams SDSS Sy2/StB experimental detachment Kauffmann et al. (1994). Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 18

Diagnostic Diagrams The BPT graphs ( Balwin, Phillips & Terlevich 1981, Veilleux & Ostrebrock 1987 ), are utilized as a part of limited line discharge frameworks, to recognize the photograph\'s roots ionization, hard and delicate radiation, which is generally attributed to non-stellar and stellar movement, individually. The general criterium [O III]/H β > 3 could not be right ! Stun warmed Power-law Sey2 Planetary nebulae LINERs H II gal H II cosmic systems (BPT 1981) (Peterson 1997) Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 19

Diagnostic Diagrams DIAGNOSTIC DIAGRAMS Em.lines in the red reach [N III ] 6584/H α versus [O III ] 5007/H β [S II ] 6717-31/H α versus [O III ] 5007/H β [O I ] 6300/H α versus [O III ] 5007/H β Em.lines in the blue reach [O II ] 3727/H β versus [O III ] 5007/H β [O II ] 3727/H β versus continuum list Other line proportions in UV , NIR and FIR ghastly ranges N V 1240/Ly α , N V 1240/He II1640 , C IV/Ly α [Si VI ] 1.962 μ m/Pa α [Ne V ] 14 μ m/[Ne II ] 12.8 μ m, [O IV ] 26 μ m/[Ne II ] 12.8 μ m, EW(PAH 7.7 μ m) Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 20

AGN scientific categorization: LINERs LINER = L ow-I onization N bolt L ine R egion They are portrayed by [O II] λ3727ã…/[O III] λ5007ã… â‰¥ 1 [O I] λ6300ã…/[O III] λ5007ã… â‰¥ 1/3 Most of the cores of close-by cosmic systems are LINERs. A registration of the brightest 250 worlds in the close-by Universe demonstrates that 50–75% of goliath systems have some powerless LINER action (Phillips et al. 1986, Ho, Filippenko & Sargent 1993, …). They are the weakest type of movement in the AGN zoo. (Heckman 1980) Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 21

AGN scientific classification: BAL QSOs BAL QSOs = B street A bsorption L ine QSOs Otherwise typical QSOs that show profound wide ingestion lines, blueward of the comparing discharge reverberation lines of C IV , Si IV , N V . The interpre-tation is that they are inborn and emerge from mists outflowing the core. They basically are at z ≥ 1.5 in light of the fact that the marvel is seen in the rest-outline UV. At these redshifts, they are ~ 10% of the watched populace. Mean QSO range PG 0946+301. Arav et al. (1999) Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 22

AGN scientific categorization: BL Lac s & Blazars BL Lacertae is the model of this class: an item, stellar in appearance, with extremely powerless emanation lines and variable, extraordinary and exceedingly captivated continuum. The frail lines frequently simply show up in the most quiet stages. BL Lacs, alongside optically brutal variable (OVV) QSOs, constitute the class of Blazars : these are accepted to be questions with an in number relativistically shot plane in the observable pathway. Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 23

AGN scientific categorization: XBONGs = X - beam B right O ptically N ormal G alaxies This AGN class comprises of brilliant hard X-beam sources facilitated by "normal" cosmic systems with optical spectra common of ahead of schedule sort frameworks (Comastri et al. 2002). Why the generally brilliant X-beam outflow, run of the mill of reasonably radiant (10 42-43 erg s - 1 ) Active Galactic Nuclei , does not leave any optical mark of the vicinity of an atomic source is still matter of civil argument. Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 24

AGN scientific classification: XBONGs as far as possible on the optical outflow lines ([O III ], H α ), anticipated from the atomic movement, in some XBONGs are sufficiently tight to put these sources outside the normal AGN properties. Conceivable understandings : Dilution from the host cosmic system light Radiatively wasteful gradual addition stream Heavy obscuration by Compton-thick atomic gas NLR clouded on universe scale (i.e., Kpc dust paths, see Malkan et al. 1998, Rigby et al. 2006 ) Extreme BL Lacs objects Hellas2XMM Marco Mignoli: AGN Optical Classification & Luminosity Function

Slide 25

AGN scientific categorization: the sort 2 QSOs Definition : “ Quasar (high L) simple of Sy2 systems ” OPTICAL : high bolometric iridescence ( → high z) objects with high ionization, slender ( FWHM<1500 km/s ) outflow lines, no expansive lines. ( anticipated that agreeing would the Unification models of AGN) X-RAYS : high-glow ( L x > 10 44 erg/cm/s 2 ) and darkened ( N H >10 22 cm - 2 ) AGN ( needed by XRB blend models ) . Do clouded (sort II ) quasars exist? To

Recommended
View more...