Quick report of the project 123 (submm follow-up)

Transcription

1 HSC-AGN f2f meeting Aug. 26, Quick report of the project 123 (submm follow-up) Takuma Izumi IoA/UTokyo 1

2 #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? (T. Izumi+) B 4 QSOs M1450 = -22.4, -23.6, -23.6, -24.9, [CII] 158μm Y Mdust, Mgas, SFR, size, σ[cii] MBH-σ next Dec?* (T. Izumi+) C (filler) 2 BAL candidates M1450 = -24.2, ~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

3 grade-c grade-b ALMA ~12.2 hrs ~13.2 hrs Matsuoka+16 3

4 Other ALMA studies on high-z quasars (1/2) ID PI Title Note S R. Assef High-Resolution [Cii] Imaging of the Most Luminous Galaxy z=4.6 Hot DOG, [CII] 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 T S. Chapman Unlensed HyLIRG systems from the South Pole Telescope 2500deg^2 survey z= HyLIRGs, [CII]+[NII], ISM physics S S. Matsushita Imaging the Molecular Gas Outflow from Gravitationally Lensed QSO MG in 20 pc Resolution (20 pc) imaging of CO(11-10); outflow properties/origin S B. Venemans Approaching the Black Hole Sphere of Influence in a Quasar at z=7.1 J @z=7.1, 0.05 = 250 pc, kinematics/sf properties 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 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 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 [CII], 1kpc view on SF (rate, size, ΣSFR vs LAGN) 4

5 Other ALMA studies on high-z quasars (2/2) ID PI Title Note S F. Stanley Radio-luminous AGN through ALMA's eyes: What is the effect of luminous radio activity on star formation? z= , SFR and ssfr distribution of RL- AGN, Radio-normal AGN, SF galaxies; (radiomode) AGN-feedback 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 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 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 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 S Y.-Y. Chang Compaction in Obscured AGN Hosts Test AGN-induced (compaction) SF scenario in 10 obscured AGNs; high-res imaging; FIR cont 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

6 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

7 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 J D, DnC ± ± ± a 3.70 ± 0.52 a 3.0 ± 0.4 a ± b 5.80 ± 1.15 b 4.6 ± 0.9 b CFHQS J W c 15 C ± ± ± ± ± 0.3 CFHQS J E 15 C ± ± ± ± ± 0.3 SDSS J D, DnC, C d 860 d ± ± ± 0.5 CFHQS J C e <0.038 <1.28 <1.0 SDSS J D 6.26 f <0.062 <2.00 <1.6 tobs = 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

8 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