Group meeting @ Nov. 01, USTC 4/18/2019 Group meeting @ Nov. 01, USTC AGN-dominated SFG-dominated

Discovery of quasar in 1963 - famous 3C 273 quasar, QSO, quasi-stellar object, ... starlike extremely luminous broad lines jet Greenstein & Schmidt 64; optical 3C 273 Bahcall+95 HST (~ B,V) + MERLIN (18 cm)

Discovery of quasar in 1963 - famous 3C 273 - SED quasar, QSO, quasi-stellar object, ... starlike extremely luminous broad lines jet UV/optical - near-IR panchromatic Courvoisier 98

Active Galactic Nuclei (AGNs) family AGN, quasar, QSO, quasi-stellar object, .. high or low luminosity Broad line or narrow line Type I or II Seyfert 1, ..., 1.5, ..., 2 FR I or II LINERs: Low-Ionization Nuclear Emission-line Regions blazars: BL Lac and Optically Violent Variables (OVVs) ...

BH + Accretion power and AGN structures more or less ... Beckmann & Shrader 2012

Radio-loud (RL) and radio-quiet (RQ) in AGN UM RL: radio-loud how and when does jet emerge? jet Elvis+94 RQ: radio-quiet Beckmann & Shrader 2012

Radio emissions synchrotron (relativistic e-) 4/18/2019 Radio emissions synchrotron (relativistic e-) supernova remnants ~ SF (Condon+13) shocks in outflows (Zakamska & Greene 14) AGN’s corona & jet free-free (bremsstrahlung) HII regions ~ SF From Vernesa Smolčić

Radio emissions and the radio-IR correlation 4/18/2019 Radio emissions and the radio-IR correlation for normal galaxies L1.4GHz LTIR ~ SFR From Vernesa Smolčić

the same mechanism for the radio emission? Are RL quasar the same population as RQ quasar? RL: radio-loud the same mechanism for the radio emission? jet Elvis+94 RQ: radio-quiet weak AGN? SF? Beckmann & Shrader 2012

What matters: RL vs RQ quasars? single vs two population(s) Why is only a small fraction, 10-15% of quasars RL?

Single population - all related to SMBH/AGN? 4/18/2019 Single population - all related to SMBH/AGN? BH mass, Accretion rate, magnetic field, BH spin (jet > RL) no evidence for BH spin powering jets in X-ray binaries? (Fender+10) the role of BH spin in powering quasar radio jets remains uncertain? (Heckman & Best 14) Intermittent activity (active > RL) characteristic timescales of months to years, amplitude <~ 1 mag Absorption (few absorption > RL) suppressed by synchrotron self absorption and/or free-free absorption Host galaxy properties (no host difference?) a mixture of early- and late-type galaxies for the host of QSOs? (...) the hosts of both RL and RQ quasars with Mi < -22.7 are all massive ellipticals? (Dunlop+03) Relativistic Doppler beaming (view along the jet > RL) radiation is beamed into a solid angle ~ 1/γ2, with typical γ ~ 10 (Scheuer & Readhead 79)

4/18/2019 Two populations? SMBH/AGN RL RQ Kellermann+89 SF

A volume-limited sample observed by VLA @ ~ 6 GHz 4/18/2019 A volume-limited sample observed by VLA @ ~ 6 GHz to compare the radio properties of optical-selected QSOs ... 178 optical color-selected QSOs: “radio-unbiased”: QSO selected using SDSS colors exclude only 1.4 GHz FIRST detection real AGN: more than one broad line with FWHM > 1000 km s-1 bright enough: Mi < -23 (or mi < 19 for z < 0.3) exclude Seyfert and low-luminosity AGNs 0.2 < z < 0.3 see also, Kimball+11, Condon+13, Kellermann+16, ...

Source properties (VLA beam width ~ 3.5″ FWHM @ ~ 6 GHz) 4/18/2019 Source properties (VLA beam width ~ 3.5″ FWHM @ ~ 6 GHz) Stotal Speak RL RQ L6 ≳ 1023.2 W Hz-1 or S ~ 0.6 mJy beam-1 for z ~ 0.3 34 RL Quasars: ~ 20% L6 ≳ 1023.2 W Hz-1 ~ 100 kpc 13 extended 144 RQ Quasars: ~ 80% 1021 ≲ L6 ≲ 1023.2 W Hz-1 SFR ~ 2 - 200 M☉ yr-1 radio size ≲ 10 kpc 1 extended (maybe unreal)

(a) 5 extended RL quasars with asymmetry - must be AGN power! 4/18/2019 (a) 5 extended RL quasars with asymmetry - must be AGN power! relativistic Doppler boosting

(a) 8 extended RL quasars with symmetry - not AGN alone! 4/18/2019 (a) 8 extended RL quasars with symmetry - not AGN alone! litter or no differential Doppler boosting

(b) Bimodal distributions? 4/18/2019 (b) Bimodal distributions? the presence of two populations the radio-loud population cannot result from the extended emission alone Stotal Speak

(c) 6 GHz radio luminosity function @ z ~ 0.2-0.3 4/18/2019 (c) 6 GHz radio luminosity function @ z ~ 0.2-0.3 RLQs: ~ 20% L6 ≳ 1023.2 W Hz-1 flat LF RQQs: ~ 80% bump at L6 ~ 1022.3 W Hz-1, or SFR ~ 20 M☉ yr-1 evidence for SF in QSO host galaxies two separate populations whose radio emission is dominated by distinctly different energy sources.

4/18/2019 Summary VLA observations of a sample of 178 SDSS QSOs with Mi < -23 and 0.2 < z < 0.3 QSO radio emission (suggested) most luminous objects ~ SMBHs less luminous objects ~ SFs relevant measure of radio loudness (more physical) radio luminosity, instead of the radio-optical flux density ratio RL: AGN > SF; RQ: SF > AGN symmetrical extended structures and flux density distribution of RL quasars relativistic beaming is no enough FAST ? & future SKA, ngVLA, ...

Existing and planned surveys @ 1.4 GHz 4/18/2019 Existing and planned surveys @ 1.4 GHz Norris+13

4/18/2019 radio future