Quasars (and AGN) with the Nuclear Spectroscopic Telescope Array (NuSTAR) Fiona Harrison Caltech

Quasars (and AGN) with the Nuclear Spectroscopic Telescope Array (NuSTAR) Fiona Harrison Caltech

INTEGRAL, Swi? BAT NuSTAR Focal spot Grazing incidence op6cs 3

Sensi6vity Satellite (instrument) INTEGRAL (ISGRI) SwiR (BAT) NuSTAR Sensi/vity ~0.5 mcrab (20-100 kev) with >Ms exposures ~0.8 mcrab (15-150 kev) with >Ms exposures 1 μcrab (10-40 kev) in 1 Ms NuSTAR two- telescope total collecbng area SensiBvity comparison 4

Broadband X- ray Emission from Accre6ng Black Holes Corona (hard X- rays) Corona (hot plasma- > hard X- rays) 5

Spectral Components flux density (arbitrary units) 0.01 0.1 1!"#$%&'%()*)++,' -.(&()'")/$0'1'2'3'' -.(&($4$%&#"%' 567(#8*()' <$'=>'4")$'' 9(,8&()' 7.(+4/$#' <$'=>? @'=> 3 ' <$'=B'' A"'=>' <$'='$/C$' 9(,8&()'.+,8' :$;$%*()'78$%&#+,' N h =2 x10 22 N h =2 x10 25 N h =2 x10 23 Hard X- ray con6nuum source dense material 2 5 10 20 50 100 Energy (kev) From PonB (2012), MaL (2003) Coronal emission: steep power law (photon index Γ~2) If dense material (disk or molecular clouds/torus)» Hard X- ray Compton bump visible 6

X- ray Obscura6on NuSTAR energy band XMM NuSTAR 7

Mrk 231: The Nearest Quasar 2 Shielding Gas (Failed Wind) Disk Wind UV Driven X-ray Corona SMBH UV Radiation 10 16 cm Accretion Disk Broad Absorp6on Line Quasars disk wind model» Fast oudlowing, line- driven winds cause broad absorp6on lines» Seen at high inclina6on» Shielding gas prevents over ioniza6on» ORen X- ray faint 8

Mrk 231 Weak Fe + hard con6nuum (Γ=1.4) but no refec6on BeppoSax Photons cm 2 s 1 kev 1 10 5 10 6 0.2 0.24 0.33 0.51 0.86 1.6 3 5.7 11 22 45 5 10 20 50 Energy (kev) Teng et al. ApJ submiled Best NuSTAR + Chandra models show N H ~ 10 23 cm - 2, no Compton hump, Γ=1.4 Absorp6on cannot explain the X- ray weakness» Related to high Eddington ra6on (a la X- ray binaries)?» Intrinsically hard coronal emission 9

Intrinsically X- ray Weak Quasars See also Luo et al. 2013 10

Obscured Quasars Required in order to explain the shape of the CXB NuSTAR Surveys» Goal: constrain evolu6on of obscura6on from z=0.1-2» Blank fields: ECDFS, COSMOS, Serendipitous sources in EG fields» SDSS obscured quasar sample Measure columns from X- ray» BAT local sample (Seyferts) 11

Constraining Obscura6on In 3-8 kev band cannot constrain columns >~few x 10 23 cm - 2» Strong suppression of sor X- ray flux across en6re band For N H < 5 x 10 24 cm - 2 10 40 kev flux unaffected Above N H = 10 25 cm - 2 broadband flux strongly suppressed (8-24 kev)/(3-8 kev) NuSTAR/XMM band ratio 10 1 SDSS J0011+0056 MYTorus model zwabs pow model 10 24 N H [atoms cm -2 ] 8 24 3 8 12

SDSS/Chandra Selected Obscured Quasars Sample selec6on» Z ~ 0.4 0.5 Vignali et al Chandra sample» L 2-10 kev/l [OIII] <2.5: factor 100 suppression of X- ray Results of first three» SDSS J0011+0056: (8-24)/(3-8) kev indicates N H =8.4+/- 3.3 x 10 23 cm - 2 (near Compton- thick)» Upper limits J0056+0032, J1157+6003 strong suppression of 8-24 kev flux: extreme Compton thick systems 13

An Obscured Quasar in ECDFS Not uniquely iden6fied as highly obscured by Chandra/XMM Extreme (8-24)/(3-8) kev ra6o iden6fies it as an obscured quasar» N H =5-6 x 10 23 cm - 2» Z~2 based on X- ray Fe- line» L 2-40 kev = 1.3 x 10 45 erg s - 1» Prominent reflec6on: R~1 (R=0 typically assumed for luminous AGN in XRB synthesis models) NuSTAR J033202-274650 14

Constraining Reflec6on in Nearby Seyferts 2MASX J16303265+3923031 5- sigma detec6on in 54- month BAT survey NuSTAR spectrum in 15 ksec 15

Broadband Studies of Seyfert Galaxies XMM NuSTAR 0 V 0 V!"#$% &%'(")$*+,t-%./#*t*nvt0+1nv V 0 k-v V 0 V V Vk 2/+'34te0+1d g Vk 0k gk 2/+'34te0+1d NGC1365 XMM+NuSTAR: Walton et al. in prep 16

Physical Condi6ons in the Corona Spectral cutoff E c ~2-3 kte Constrain electron temperature, op6cal depth IC4329A: kt = 50(+0.9/- 0.5_ kev, τ=1.5 MCG- 5-23- 16: 17

Baseline Mission Science Science Group Galac6c Surveys, Galac6c Center Supernovae and ToOs Supernova remnants and Pulsar Wind Nebulae Magnetars and Rota6on Powered Pulsars Galac6c Binaries Ultraluminous X- ray Sources Extragalac6c Surveys Blazars and Radio Galaxies Obscured AGN AGN Physics Galaxy Clusters Starburst Galaxies Solar Physics Working Group Chair Chuck Hailey Steve Boggs Fiona Harrison Vicky Kaspi John Tomsick Fiona Harrison Daniel Stern Greg Madejski Daniel Stern Giorgio May Allan Hornstrup, Silvano Molendi Ann Hornschemeier David Smith hyp://www.nustar.caltech.edu (look under for astronomers ) 18

Summary NuSTAR is working well on orbit» Several 100- fold improvement in sensi6vity over previous hard X- ray missions Providing new probes of obscured quasars and physics of Seyfert galaxies Up to 1.5 Msec of NuSTAR 6me is offered joint with XMM in AO13 Analysis sorware released with HEADAS_v6.14 NuSTAR public archive is open 19