HSC-AGN f2f meeting Aug. 26, 2016 @IPMU/Tokyo Quick report of the project 123 (submm follow-up) Takuma Izumi IoA/UTokyo 1
#123 Investigation of rest-frame far-ir to submm properties of z = 6-7 QSO-host galaxies Significant progress in this year 2 ALMA proposals (Band 6 ~ 250 GHz) are accepted! PI: T. Izumi (Univ. of Tokyo) takumaizumi@ioa.s.u-tokyo.ac.jp Follow-up SHELLQs quasars (Y. Matsuoka+16) Lower luminosity quasars at z = 6-7 *According to the current array configurations ID Grade Target z Line Rest-FIR cont. Goal (what to measure?) When to be observed? 2016.1.01423 (T. Izumi+) B 4 QSOs M1450 = -22.4, -23.6, -23.6, -24.9, 5.9-6.4 [CII] 158μm Y Mdust, Mgas, SFR, size, σ[cii] MBH-σ next Dec?* 2016.1.01487 (T. Izumi+) C (filler) 2 BAL candidates M1450 = -24.2, -23.6 ~6.4, ~6.8 [CII] 158μm Y exact-z, Mdust, Mgas, SFR, size, cold outflow next Dec?* TI s impression from the reviewer s report Determining MBH can be very crucial to obtain ALMA time NIR follow up is also the key for us 2 2
grade-c grade-b ALMA ~12.2 hrs ~13.2 hrs Matsuoka+16 3
Other ALMA studies on high-z quasars (1/2) ID PI Title Note 2016.1.00184.S R. Assef High-Resolution [Cii] Imaging of the Most Luminous Galaxy z=4.6 Hot DOG, [CII] 2016.1.00226.S R. Decarli A comprehensive study of the interstellar medium 830 Myr after the Big Bang z = 6.4 luminous QSO, 17 ionized/atomic/mol., ISM physics 2016.1.00236.T S. Chapman Unlensed HyLIRG systems from the South Pole Telescope 2500deg^2 survey z=4.2-5.7 HyLIRGs, [CII]+[NII], ISM physics 2016.1.00281.S S. Matsushita Imaging the Molecular Gas Outflow from Gravitationally Lensed QSO MG 0414+0534 in 20 pc Resolution 0.037 (20 pc) imaging of CO(11-10); outflow properties/origin 2016.1.00417.S B. Venemans Approaching the Black Hole Sphere of Influence in a Quasar at z=7.1 J1120+0641@z=7.1, 0.05 = 250 pc, kinematics/sf properties 2016.1.00668.S T. Diaz-Santos Constraining the Properties of the Interstellar Medium of the Most Luminous Galaxy in the Universe z=4.6 Hot DOG, [OI] + [NII], ISM properties 2016.1.00718.S F. Fiore The cradles of giant galaxies: the ALMA view of the most powerful QSOs in the Universe z~4.5 two WISE/SDSS QSOs, kinematics (interaction, outflow), SFR properties 2016.1.00735.S C.M.Harrison Spatially-resolved star formation at high-z; are AGN host galaxies special? (some may be missed,,) (L,z)-matched AGNs vs non-agns @z=1.5-5, [CII], 1kpc view on SF (rate, size, ΣSFR vs LAGN) 4
Other ALMA studies on high-z quasars (2/2) ID PI Title Note 2016.1.00804.S F. Stanley Radio-luminous AGN through ALMA's eyes: What is the effect of luminous radio activity on star formation? z=1.5-3.2, SFR and ssfr distribution of RL- AGN, Radio-normal AGN, SF galaxies; (radiomode) AGN-feedback 2016.1.01012.S E. Treister Gas Contents of the Host Galaxies of z>3 X-ray Selected AGN in COSMOS FIR dust cont. measurement ( Mdust, Mgas); 27 X-ray detected obscured AGNs@z>3; compare with normal galaxies 2016.1.01063.S C.D. Ferkinhoff Studying star formation via the [OI] 63 micron line within a billion years of the Big Bang Three z>6 QSOs w/ [CII] detections; [OI]; ISM properties 2016.1.01311.S Y. Kim Quasar Feedback in the Early Universe: Lowest Eddington Ratio Quasar at z~6 z~6 low-edd. ratio QSO; FIR cont.; compare with high-edd. QSOs@similar-z 2016.1.01326.S M.Schramm Unifying Stars and Gas in Quasar Hosts at z~3 and the Co-Evolution Picture z~3 QSOs (showing various NLR properties) with MBH + M*; Mgas, Mdyn future evolution 2016.1.01355.S Y.-Y. Chang Compaction in Obscured AGN Hosts Test AGN-induced (compaction) SF scenario in 10 obscured AGNs; high-res imaging; FIR cont. 2016.1.01515.S P. Lira Revealing Major Mergers Among the Extreme Star Forming Hosts of the Fastest Growing Super-Massive Black Holes at z=4.8 z~4.8 AGN (that will become MBH>10 10 Msun before z~4); [CII]; kinematics (merger? secular?) (some may be missed,,) 5
My impression on the outcome The uniqueness of our sample is outstanding! - The referees did understand the importance of these projects The knowledge of MBH is critical to achieve telescope time(s). 6
Discussion item (1/2): Other telescopes For example, CO(2-1) measurement with JVLA molecular mass, SFR, kinematics Observations Wang+11 Name t obs Configuration Redshift FWHM I v L CO(2 1) M gas (hr) (km s 1 ) (Jykms 1 ) (10 10 K km s 1 pc 2 ) (10 10 M ) (1) (2) (3) (4) (5) (6) (7) (8) SDSS J092721.82+200123.7 20 D, DnC 5.7716 ± 0.0012 590 ± 130 0.129 ± 0.018 a 3.70 ± 0.52 a 3.0 ± 0.4 a 0.202 ± 0.040 b 5.80 ± 1.15 b 4.6 ± 0.9 b CFHQS J142952.17+544717.6W c 15 C 6.1831 ± 0.0007 280 ± 70 0.065 ± 0.011 2.06 ± 0.35 1.6 ± 0.3 CFHQS J142952.17+544717.6E 15 C 6.1837 ± 0.0015 400 ± 140 0.050 ± 0.013 1.59 ± 0.41 1.3 ± 0.3 SDSS J084035.09+562419.9 20 D, DnC, C 5.8441 d 860 d 0.062 ± 0.022 1.81 ± 0.64 1.4 ± 0.5 CFHQS J021013.19 045620.9 15 C 6.438 e <0.038 <1.28 <1.0 SDSS J162331.81+311200.5 20 D 6.26 f <0.062 <2.00 <1.6 tobs = 15-20 hrs (for M1450 ~ -26 objects) Unrealistic to follow-up SHELLQs QSOs (M1450 ~ -23) under a fixed L CO/LAGN Strongly depends on the ratio Our Cy4 results will be the key? But it s OK to follow-up some specific ones? 7
Discussion item (2/2): ALMA itself tobs is large for each object (a few hrs), as our samples are predicted to be faint at [CII] and FIR - current estimate; scaled from luminous QSOs MBH is (much) better to be known - NIR follow-up must be the key Hard to follow-up *all* SHELLQs-QSOs with annual ALMA observations(?) (1) Regular proposal (selected targets)? relatively deep, individual detection (2) Regular proposal (many targets)? relatively shallow, but stack? (3) Large proposal? (quite a hard task) Better? 8