DISK AND JET PARAMETERS IN FLAT SPECTRUM RADIO

Lyuba Slavcheva-Mihova Boyko Mihov Institute of Astronomy and NAO, Bulgarian Academy of Sciences

Where is the difference?

A couple of 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 (3C 273) vs. a quiescent elliptical

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 ' 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)/(16πσR )][1–(3RS/R) ]

• It peaks at R≈4RS, so, the Schwarzschild radius could be found as: 4 4 RS = (0.14 LAD)/[πσ(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

br − break enerμy q – high-energy spectral index

Modeling details

The SEDs were modeled using the SSC/EC Simulator developed by Tramacere at the ASI Science Data Center. • To decrease the number of parameters we held fixed Γ and to the observed values from SL measurements (for 12 of the objects). For some of the sources, however, better fits were obtained by varying and then computing Γ = 1/.

• BLR and DT radii were calculated from LAD each time the latter changed. • The AD parameters are well constrained by the SED bump near log()=15. • The slope q of N() is constrained by the WISE mid-IR data • br is constrained by the -ray data. Fitted SED of the source 2230+114

The individual emission components are specified. Results

Model parameter (min, median, max): Emitting blob: Electron energy distribution:

× 16 × 16 × 17 • R: 2.2 10 , 5.5 10 , 1.3 10 cm • min :1, 1, 9

• B: 0.9, 3.4, 10.0 G • br: 15, 90, 500

• Γ: 12.3, 18.4, 27.9 • : 30000, 52500, 100000 max

• : 2.5, 3.4, 5.7 degrees • p: 1.00, 2.10, 2.90

• q: 3.10, 3.38, 4.02 Results: AD, BLR, DT

45 46 47 -1 • LAD: 1.0×10 , 2.5×10 , 2.0×10 erg s

• TAD,peak : 20000, 26000, 40000 K

17 17 18 • RBLR: 1.00×10 , 6.25×10 , 1.00×10 cm

18 18 19 • RDT: 2.5×10 , 7.9×10 , 3.5×10 cm

• These parameters are in good agreement with the ones derived for other samples of FSRQs, e.g., Ghisellini et al. 2010.

Pjet & LAD

-1 -1 log(Pjet): 45.8, 46.9, 47.5 erg s log(LAD): 45.0, 46.4, 47.3 erg s Jet Parameters

• Ljet/Pe = 4.9 Pp/Ljet = 3.3 LEC,BLR /LSyn: 1.5, 10.7, 80.9

• Ljet/Pjet = 0.05 • There is no significant difference between LPQ and HPQ

red – LPQs, blackHPQ – –HPQs hatched LPQ – blue

– LPQ □HPQ – • •LPQ – HPQ – □ Disk-Jet Connection

Ljet/LAD = 0.1 LAD/Pjet = 0.3

LPQ tend to have more luminous ADs ...

HPQ – • LPQ – □

HPQ – • LPQ – □ Accretion -1 LAD: 0.01, 0.05, 0.14 LEdd Ṁin = 0.2, 4.4, 35.3 Mʘ yr Ṁin = 0.1, 0.5, 1.4 ṀEdd

... and higher accretion rates.

red – LPQs, red – LPQs, blackHPQ – HPQs – hatched blackHPQ – HPQs – hatched LPQ – blue LPQ – blue Black hole masses: distribution

8 9 10 •MBH (min, med, max): 3.9 × 10 Mʘ, 3.1 × 10 Mʘ , 1.1 × 10 Mʘ

•The black holes in LPQs seem to be larger.

red – LPQs, HPQ – • HPQ – hatched black – HPQs LPQ – □ LPQ – empty LPQs vs. HPQs

Values of LAD, Ṁin and MBH for LPQs are larger than for HPQs. In the framework of the Blazar Sequence: a well defined continuous sequence in the observed spectral properties of blazars even on smaller scales encompassing FSRQs subtypes, so that the transition HPQs → LPQs is accompanied by an increasing importance of the external radiation field, which inevitably influences the FSRQ classification.

'SED' MBH: comparison with literature data

Source: MBH: Reference: 9 0106+013 ... 3×10 Mʘ... this work 9 5×10 Mʘ ... Ghisellini et al. // 2011 MNRAS, 411, 901 9 1226+023 ... 5×10 Mʘ... this work 8 (3C 273) 8×10 Mʘ ... Ghisellini et al. // 2010 MNRAS, 402, 497 9 6.59×10 Mʘ ... Jolley et al. // 2009 MNRAS, 400, 1521 9 1510-089 ... 1×10 Mʘ ... this work 8 7×10 Mʘ ... Ghisellini et al. // 2010 MNRAS, 402, 497 8 5.4×10 Mʘ ... Abdo et al. // 2010 ApJ, 721, 1425 9 2230+114 ... 2×10 Mʘ ... this work 9 1×10 Mʘ ... Ghisellini et al. // 2010 MNRAS, 402, 497 Good agreement among different estimates apart from 3C 273. 3C 273

9 MBH = 6.59×10 Mʘ ... Jolley et al. 2009 8 8×10 Mʘ ... Ghisellini et al. 2010 9 5×10 Mʘ... this work – AD – well constrained • possible host galaxy contribution that does not influence the AD

2134+004 : the record-holder

10 MBH =1.1 × 10 Mʘ left 10 MBH =0.9 × 10 Mʘ right

• possible host galaxy contribution that may influence the AD

Largest MBH: alternative models

• Schwarzschild vs. Kerr BH

• The derived MBH are larger when considering a Kerr BH (Jolley et al. 2009; Ghisellini et al. 2010) • An isotropic standard (optically thick, geometrically thin) AD

• slim super-Eddington disk, with Ṁin ~ ṀEdd, no strong collimation, a modified BB emission (Abramowicz et al. 1988) • a thick disk - a collimating funnel - the impression of a super- Eddington luminosity (Jaroszynski et al. 1980)

• Both can reduce the MBH estimate, but produce bluer spectra (Ghisellini et al. 2009, 2010) • a BB emission at each radius

• a conservative assumption => a lower limit to MBH

Largest MBH ...

• A BB emission at each radius

• a conservative assumption => a lower limit to MBH

10 0014+813, − − radio-loud quasars with MBH > 10 Mʘ • the jet can play a crucial role in the angular momentum transfer, allowing the BH to grow faster (Jolley & Kuncic 2008) • Caveats: • Lyα absorption beyond z > 2 • host galaxy contribution → → → • simultaneous data needed

Black hole masses: SED vs. virial

• Our MBH estimates are about 6 times larger then the virial ones.

HPQ – • □ – LPQ LPQ – □ • – HPQ Virial Method Uncertainties

• BLR geometry and inclination; • the role of radiation pressure; • tνe modelinμ of emission line profiles; • the contribution from other components (e.g. host galaxy); • whether gravity dominates the motions of the BLR clouds;

• Systematic difference in MBH estimated on line & continuum L in the optical/UV due to the contribution of the synchrotron emission.

SED vs. virial mass estimation

2 1. Virial technique: MBH = RV /G, V = f FWHM f – depends on the BLR model • for isotropic velocity distribution f = (3/4)0.5; • for disk-like geometry f depends on the viewing angle and on the disk thickness: f = 0.5/[(H/R)2+sin2θ]0.5; • in the limit of f = 0.5/sin θ.

2. Independent estimate of f: 2 2 • f = (MBH G)/(R FWHM ) if we measure R, FWHM, and independently MBH. SED vs. virial mass estimation

• Independent MBH estimate is taken from our SED modeling; • We got median f = 5.9 ± 2.7 (st.dev.) • this supports a disk-like geometry of the BLR • If we assume a thin disk model for BLR, then the median value of the angle between the line of sight and the rotation axis is = 4.9˚.

• Decarli et al. (2011) found • < f > = 5.6 ± 1.3 for blazars

• < f > = 2.0 ± 0.3 for quasars using MBH derived from the mass of the host galaxies. 3C 273: half a century later The evening of Febr. 5, 1963 – one man only knows that 3C 273 is not an ordinary star in our but a powerful object

at DL = 749 Mpc! The puzzle was suddenly resolved in the afternoon of Febr. 5, 1963, ... I decided to check the regular spacing of the lines by taking the ratio of their wavelengths to that of the nearest line of the Balmer series. The first ratio, that of the 5630 line to H, was 1.16. The second ratio was also 1.16. When the third ratio was 1.16 again, it was clear that I was looking at a Balmer spectrum redshifted by 0.16... Maarteen Schmidt ______

Happy Anniversary, 3C 273!