DISK AND JET PARAMETERS IN FLAT SPECTRUM RADIO QUASARS
Lyuba Slavcheva-Mihova Boyko Mihov Institute of Astronomy and NAO, Bulgarian Academy of Sciences
Where is the difference?
A couple of galaxies matched on redshift, inclination, Hubble type • UGC 6520 Mrk 766
10 44 -1 15 49 -1
•LG < 10 Lʘ (<10 erg s ) LAGN < 10 Lʘ (<10 erg s ) The bluer, the active! active! the bluer, The SEDs of different galaxies
• 1% of galaxies host AGNs • 10% of AGNs – radio-loud, able to launch jets • Although first discovered in the radio, jets emit most in the otνer extreme of tνe EM spectrum − in tνe γ-ray • a blazar (3C 273) vs. a quiescent elliptical galaxy
AGN model • AD around a SMBH, DT, BLR, NLR, eventually jet. • Unified Scheme depending on the viewing angle & jet presence
• Radio-loud AGNs: Radio-loudness parameter f(5 GHz)/f (4400 Å) > 10
Blazars
Jet-on AGNs
• Variable, at all frequencies, especially at νiμν enerμies. • Minimum variability timescales − weeks and tens of minutes. • In restricted frequency ranμes, tνeir spectrum is a power law. • Tνe variability may be coordinated in different enerμy bands • Tνey are often polarized, in tνe radio and in tνe optical. • Tνe νiμν enerμy νump often dominates tνe power output.
Blazar SED: Synchrotron + Inverse Compton radiation
LC νC
LS ν S
BL Lac vs. FSRQs
BL Lac: absent or weak em. lines with EW < 5 Å FSRQ: strong em. lines with EW > 5 Å • Luminosity divide: 47 -1 Lγ,BLLac < 10 erg s < Lγ,FSRQ • Different accretion regimes: -2 • BL Lac radiatively inefficient L/LEdd < 10 , Ṁ/ṀEdd < 0.1 -2 • FSRQ radiatively efficient L/LEdd > 10 , Ṁ/ṀEdd > 0.1
• New classification -3 BL Lac: LBLR/LEdd < 10 -3 FSRQ: LBLR/LEdd > 10
Other blazars' classifications • Low/Intermediate/High synchrotron peaked 14 15 • LSP ( S < 10 Hz) → ISP → HSP → ( S > 10 Hz) • Almost all FSRQs are LSP
• Low-/High-frequency BL Lac (radio/X-ray spectral index RX )
• LBL: RX > 0.75 – IR-opt; HBL: RX < 0.75 – UV-X-ray • Low-/High-polarization FSRQs (fract. lin. opt. polarization p) : • LPQ: p < 3%; HPQ: p > 3% on at least one occasion
HSP, Mrk 421 LSP, PKS 123 510-089 Blazar Sequence
FSRQ
BL Lac LBL IBL HBL Blazar Sequence
• Low-power blazars (i.e., BL Lacs), are bluer (the peak frequencies of both peaks are larger) than powerful ones (FSRQs). • The high energy hump increases its relevance as we increase the bolometric luminosity. At low luminosities both humps have the same power, while the most powerful FSRQ have a high energy hump that is 10 times the low energy one.
∼ • Since FSRQs have stronger emission lines, the seed photons are more and thus produce stronger high energy hump. • More seed photons in FSRQs → stronger radiative cooling → the SED peaks in the FIR and MeV bands.
BH mass estimation methods
• Reverberation mappinμ RM − based on tνe time delay bet. the variability in the em. lines & continuum • One of the most accurate BLR size estimation methods • highly time-consuming, • sinμle epocν virial metνod SE virial – RM-calibrated scaling relations (Peterson 1993; Bentz et al. 2009) based on empirical connection between the BLR radius and the source monochromatic luminosity • simple applicability Aims and sample selection • To explore the disk-jet connection through the relations among their parameters, focusing on the disk parameters, and esp. the
BH mass MBH. FSRQs are most suitable as: • their AD signatures are better expressed • they have SE virial black hole mass estimates • We selected FSRQs with:
• SE virial MBH estimates from the compilation of Zhou & Cao usinμ publisνed FWHM Mμ II, H , or H and & L (the line or the opt./UV continuum) data • As dense as possible coverage of the SED, excluding at the same time strongly variable SEDs • Well pronounced AD optical-UV bump
• Out of the 78 sources with measured MBH we selected 14 FSRQs that best meet the selection criteria.
Name Class. z List of sources 0016+731 LSP LPQ 1.781000 0106+013 LSP HPQ 2.099000 0112-017 * LPQ 1.365000 0212+735 LSP HPQ 2.367000 0336-019 LSP HPQ 0.852000 0420-014 LSP HPQ 0.916087 0440-003 LSP HPQ 0.844000 0736+017 LSP HPQ 0.189410 1226+023 LSP LPQ 0.158339 1510-089 LSP HPQ 0.360000 2128-123 LSP LPQ 0.501000 2134+004 LSP LPQ 1.932000 2155-152 LSP HPQ 0.672000 2230+114 LSP HPQ 1.037000 SED
• SEDs were built using non-simultaneous data from the ASI Data Center. • We want to study the objects of interest as a population – not so many alternative options • Constraints on the parameters from other studies (e.g. Γ & ) • An advantage of our work over the previous studies is the presence of WISE (mid-IR 3-50 m or log( )=13-14) data, which tightly constrain the slope of the synchrotron part of the SED. • On some SEDs the signature of the host galaxy could be found. • As an example - SED of the source 2230+114 (a.k.a. CTA 102); catalogues used for its construction are labeled. SED of the source 2230+114 Model
• One-zone leptonic Syn+IC (IC=SSC+EC) model with self- absorption included; • EC=EC(BLR)+EC(DT)
• Homogeneous spherical blob of radius R, moving with a bulk Lorentz factor Γ at a viewing angle with tangled and uniform magnetic field of intensity B.
AD • A standard (optically thick, geometrically thin) AD around a Schwarzschild BH (Shakura & Sunyaev 1973) with
parameters LAD, TAD,peak.
• Temperature profile of AD: 4 3 0.5 T (R) = [(3RSLAD)/(16π σR )][1–(3RS/R) ]
• It peaks at R≈4RS, so, the Schwarzschild radius could be found as: 4 4 RS = (0.14 LAD)/[π σ(TAD,peak ) ], where we use =0.1;
2 • The black hole mass can be derived as MBH = (RSc )/(2G), 2 • and the accretion rate as Ṁ = LAD/( c )
BLR & DT • Broad Line Region: 17 45 0.5 • RBLR = 10 (LAD/10 ) cm, • Bentz et al. 2006; Kaspi et al. 2007; Bentz et al. 2009
• Dusty Torus: 18 45 0.5 • RDT = 2.5×10 (LAD/10 ) cm
• TDT < 1500 K
• We assume:
• LBLR = 0.1LAD
• LDT = (0.1-0.3)LAD
• TDT ~ 370 K Energy distribution of the emitting electrons
Broken power law distribution of the emitting electrons defined in the interval [ min, max]: –p N( ) ~ for min < < br –q N( ) ~ for br < < max p – low-energy spectral index