Luminous Quasars and AGN Surveys with ELTs

Transcription

1 Luminous Quasars and AGN Surveys with ELTs Roberto J. Assef Núcleo de Astronomía Universidad Diego Portales

2 This Talk Will focus on two topics: 1. The most luminous (obscured) quasars 2. AGN surveys Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 2

3 Most Luminous AGN ( L ) Many different types have been discovered Not clear how they relate to each other Luminous Type 1 QSOs (e.g., SDSS, Richards et al. 2006, Ross et al. 2013) Luminous Reddened Type 1 QSOs (e.g., Banerji et al. 2015) WISSH quasars (SDSS+WISE, Bischetti et al. 2017) Extremely Red Quasars (ERQs, Hamman et al. 2017, Ross et al. 2017) Hot Dust Obscured Galaxies (Hot DOGs, Eisenhardt et al. 2012) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 3

4 Eisenhardt et al. (2012) [3.4] [4.6] [4.6] [12]

5 Hot DOGs are at High-z and are Hyper-Luminous Assef et al. (2015) Identified by WISE All at z>1 Low contamination rate of selection by low-z interlopers Hot DOGs All have L IR >10 13 L 10% have L IR > L Intrinsic, no lensing 1 per 30 sq. deg. Very rare! Comparable to type 1 and red quasars Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 5

6 Hot DOGs are at High-z and are Hyper-Luminous Identified by WISE All at z>1 Low contamination rate of selection by low-z interlopers All have L IR >10 13 L 10% have L IR > L Intrinsic, no lensing 1 per 30 sq. deg. Very rare! Comparable to type 1 and red quasars Tsai et al. (2015, ApJ, 805, 90) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 6

7 Hot Dust Obscured Galaxy Hot DOG First object studied in detail (Eisenhardt et al. 2012, 755, 173) Best fit SED model has AGN with A V ~ 50 mag Starburst with ~300 M sun /yr SFR L Bol = 9 x L Adapted from Eisenhardt et al.(2012) July Cambridge Roberto J. Assef - UDP 7

8 Remarkably Similar SEDs Tsai et al. (2015, ApJ, 805, 90) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 8

9 Hot DOGs and Host Galaxies Very luminous AGN, in not so massive galaxies Somewhere between two limits (Assef et al. 2015) a) Very massive SMBHs for their hosts b) Very high Eddington ratios Regardless of which, these objects may be great pleases on which to observe feedback in progress Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 9

10 Ionized Gas Outflows Hot DOGs Jun, Assef et al. in prep XSHOOTER spectra Outflows are very common Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 10

11 Ionized Gas Outflows - WISSH Bischetti et al. (2017) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 11

12 Ionized Gas Outflows - ERQs Zakamska et al. (2016) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 12

13 Outflows with Next Gen Telescopes Better spatial resolution will allow to better understand where the outflows are coming from physically Spatial differences between different lines, like [OIII] and [OII] for example. Currently, we can only detect the most powerful outflows in a few very strong lines. Fainter outflows Other transitions for a more complete physical picture Better match to ALMA resolution Better connect ionized and molecular outflows Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 13

14 Isotropic outflow in Hot DOG W ? z = Diaz-Santos et al. (2016, ApJL, 816, 6) L Bol = 3x10 14 L Most luminous Hot DOG FWHM is about 600 km/s L [CII] = 6 x 10 9 L Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 14

15 Diaz-Santos et al. (2016, ApJL, 816, 6) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 15

16 W2246 Dust Continuum Diaz-Santos et al. (2018, Science, 362, 1034) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 16

17 Next Gen Telescopes Probe Mergers Features in Depth First time such merger features are detected But little search done prior to W2246 detection ALMA detection of dust emission implies SF in the tidal features Dust heating unlikely to be only due to the quasar Undetected to HST so far Could be detected with deeper HST or JWST perhaps Need EELTs to characterize in detail Measure stellar mass Constrain on-going star-formation rate Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 17

18 Next Gen Telescopes Relation between Populations Luminous AGN are very brief moments in a galaxy lifetimes How different classes of luminous AGN relate may be simply a matter of when we are looking James Mullaney: AGN should be thought as weather. ELTs/JWST can better constrain the host properties ELTs/JWST can better probe the environments Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 18

19 Assuming the M-! relation holds at high redshift Unlikely to hold, but provides a good rough idea M 10 9 M 10 8 M Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 19

20 Environments of Hot DOGs Gonzalez, Assef et al. in prep Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 20

21 Environments of Hot DOGs Jones et al. (2014) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 21

22 Trakhtenbrot et al. (2017) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP Decarli et al. 22 (2017)

23 AGN Surveys Long history for AGN surveys Done at every wavelength range Optical, such as SDSS, PG, etc. Mid-IR, mainly with Spitzer and WISE Xrays and radio with many facilities Every wavelength finds different populations See Padovani et al. (2017) review! Largest ones contain up to ~few million sources Milliquas The WISE-based catalogs erosita Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 23

24 WISE AGN Catalog Assef et al. (2018, ApJS, 234, 23) Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 24

25 LSST All LSST Id. XDQz R90 Assef et al. erosita Secrest et al. Milliquas SDSS DR12 Quasar Cat. ROSAT 2XRS 25

26 AGN Surveys LSST will revolutionize this in terms of number of sources Particularly with Euclid LSST identify find 20 million AGN LSST will detect but not identify >10x more This is likely to open new windows into AGN activity Lack of spectroscopy however severely hinders the results Photometric redshifts for AGNs are typically very bad, >0.1 * (1+z) Missed AGN not random Obscuration Host dilution, ~Eddington ratio Unexpected findings Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 26

27 AGN Surveys with ELTs Characterize in depth LSST sources Spatial resolution and NIR can further identify AGN photometrically Spectroscopy will become feasible Planned MOS capabilities are ideal Could try deeper photometric surveys Issues of host dilution and obscuration may make this less appealing If efficient mid-ir possible, we can really complete a lot about the AGN picture Unfortunately ELTs sites not ideal for deep mid-ir NEOCAM may help to some extent JWST, but not efficient for surveys Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 27

28 Conclusions ELTs will be great for AGN science In luminous quasars, ELTs will Probe host galaxies in detail, at least for obscured sources Probe environments to unique level of details Complete the picture about environments and mergers that is being discovered by ALMA For surveys, ELTs will Spectroscopically probe to the depth of stacked LSST Identify AGN in a less biased way Carry out even deeper surveys Big Eyes Meeting, UCLA 2019 Roberto J. Assef - UDP 28