Jan. 6 th, 2016 HSC/AGN meeting Next DL = 21 April High-z QSO follow-up @mm/submm (HSC #123) - especially z > 6 objects - Takuma Izumi@IoA/UTokyo takumaizumi@ioa.s.u-tokyo.ac.jp This is a submm follow-up study for high-z (z > 6?) QSOs uncovered by Matsuoka et al. w/ HSC 1
QSOs at z > 6 followed-up at mm/submm (incomplete) Object z MBH M1450 Ref. Lines FIR Cont. Ref. J1120+0641 7.08 2.0E+09-26.6 Mortlock+11 [CII] Y Venemans+12; De Rosa+14 J2348-3054 6.89 2.1E+09-25.7 Venemans+13 [CII] Y Venemans+16 J0109-3047 6.75 1.5E+09-25.5 Venemans+13 [CII] Y Venemans+16 J0305-3150 6.61 1.0E+09-26.0 Venemans+13 [CII] Y Venemans+16 J036.5078+03.0498 6.53 1.9E+09-27.4 Venemans+15 [CII], H2O(?) Y Banados+15 J0210-0456 6.44 8.0E+07-24.3 Willott+10 [CII], CO(2-1)* Y Wang+11; Willott +13,15; J1148+5251 6.42 4.9E+09-27.8 Fan+03; Willott+03 [CII],[NII]*, [CI],CO(2-1),CO(3-2), CO(6-5), CO(7-6) Y Bertoldi+03a,b; Maiolino+05,12; Walter+03,04,09; Riechers+09; Cicone+15;Stefan+15 J2329-0301 6.42 2.5E+08-25.0 Willott+10 [CII]* N Willott+13 J1048+4637 6.23 - -27.6 Fan+03 CO(3-2), CO(6-5) Y Bertoldi+03a; Wang +10 J2229+1457 6.15 1.2E+08-24.5 Willott+10 [CII] N (marginal) Willott+15 J1319+0950 6.13* 2.1E+09* -27.1 Mortlock+09 [CII], CO(6-5) Y Wang+11,13 J2054-0005 6.06 9.0E+08* -26.2 Jiang+08 [CII], CO(6-5) Y Wang+10,13 J1630+4012 6.05 - -26.1 Fan+03 - N Bertoldi+03a J0055+0146 6.01* 2.4E+08-24.5 Willott+10 [CII] Y Willott+15 J2310+1855 6.00* 2.8E+09* 19.3 (apparent) Fan+? [CII], CO(6-5) Y Wang+13 Note * = [CII] derived * = Edd. limited mass * = non-detection 2
Science Case (1) [CII] Wang et al. detection z = 6.0 As can be seen in the previous page, we can expect the detection of [CII] at high significance even at z > 6 (it s so bright!). 1σ = 0.5 mjy @dv=60km/s, t~1hr, # of antenna~20 rotation Although, the detection of [CII] itself can have a high priority,,, Figure 1. We show 1900 GHzet(158 µm) continuum A) and moment maps (as labelled; panels B D) of the [C II] line of J1554+1937. The grey dashed Wang al. 2013, ApJ, 773, (panel 44 contours show the continuum profile in each panel (the colour-scale and contours in panel A are equivalent). The filled grey ellipse indicates the shape and orientation of the synthesized beam (analogous to point spread function in optical/ir observations). The emission shown in panels (C) and (D) is restricted to regions where the S/N in the [C II] data cube is greater than 4. How large is the spatial extent?? - typically, it shows a compact (a few One theory put forth to explain the large blueshift in broad, highkpc) SF-region. ionization lines like C IV is commonly referred to as the disc-wind J1554+1937 double-horn rotating disk Kimball et al. 2015, MNRAS, 452, 88 Figure 2. ALMA detection of [C II] line in J1554+1937. The rms variation (determined from line-free channels) is approximately 2 mjy. Observed model (Sulentic, Marziani & Dultzin-Hacyan 2000b; Richards et al. 2011). According to this picture, the line is emitted from a radial outflow whose far side is obscured by the accretion disc, and thus only the blueshifted component is visible. The wind may arise from the disc itself. We wish to emphasize this caveat to future ALMA observers: in the submillimetre regime, such velocity offsets can amount to shifts of 1 GHz in the observed frame, potentially moving a targeted submillimetre line halfway across one of ALMA s 2-GHz-wide spectral windows. If the redshift of a QSO is known only from the (restframe) UV lines, optical emission lines, we therefore recommend that ALMA observers place multiple spectral windows alongside 3 each other to allow for an unknown, but potentially quite large, shift Does the [CII]-emitting gas show a rotating motion? Or, highly turbulent motion (e.g., merger)?? - many works assume bulge-like structure, but there is no necessity for that assumption (it can be disky).
MBH [Msun] z ~ 6 or higher Willott et al. 2015, ApJ, 801, 123 Science Case (2) Co-evolution at high-z Previous measurements of M-σ relation suggested overmassive SMBH at high-z relative to the locally-defined relation at fixed σ (e.g., Wang et al. 2010, ApJ, 714, 699). σ [km/s] The Astrophysical Journal, 770:13(7pp),2013June10 LFIR [Lsun] Willott et al. 2013, ApJ, 770, 13 LBol [Lsun] Figure 2. Far-infrared luminosity vs. AGN bolometric luminosity for z 6 quasars. The two CFHQS quasars observed with ALMA in this paper are shown But recent, improved estimation of σ Willott, Omont, & Bergeron z 6 quasars. (accounting Symbols as for Figure 6. for The black both line withdisk gray shading and is the local galaxies bulge correlation with 1the s scatter lowest froml the FIR work at a of given Kormendy L Bol are & Ho expected (2013) equating to have M dyn a to significant M components) bulge. Thefraction CFHQS quasars of their lie on L local relationship and do not show the large offset displayed by the yields FIR due to quasar-heated dust (Netzer et al. 2007). most massivethe black holes. same Uncertainties mean of Figure in M the dyn have 2 shows not been previously calculated due published to the reasons datagiven for individually the text. detected z high-z 6 quasarsm-σ and stacked as that averagesof from Wang local one, et al. (2011a) andomontetal(2013). Thedottedlineisthe whereas the scatter is considerably relationship between L FIR and L Bol found by Wang et al. (2011a) for stack averages of quasars at 2 <z<7. Note that both the larger! stacked averages and the relationship from Wang et al. (2011a) have been renormalized according to the bolometric correction adopted here (see Omont et al. 2013 for more details). Gray crosses are a complete sample of low-redshift (z <0.5) optically selected This Palomar Green suggests (PG) quasars that (Haotheir et al. 2005). host L FIR forgalaxies PG quasars has been estimated as 2 the luminosity at 60 µm (Lawrence would et al. 1989). have Note that undergone many of the highest luminosity considerable (most distant) quasars in the PG sample are undetected at 60 µm and evolution only have upper limits to onachieve L FIR. As noted by large Wang etstellar al. (2011a), the z 6stackedaverageslieclosetothecorrelation mass. 4 exhibited by low-redshift quasars, indicating no enhancement in SFR at high redshift for a given quasar luminosity.
MBH [Msun] Willott et al. 2015, ApJ, 801, 123 σ [km/s] The Astrophysical Journal, 770:13(7pp),2013June10 LFIR [Lsun] Willott et al. 2013, ApJ, 770, 13 LBol [Lsun] z ~ 6 or higher Figure 2. Far-infrared luminosity vs. AGN bolometric luminosity for z 6 quasars. The two CFHQS quasars observed with ALMA in this paper are shown Science Case (2) Co-evolution at high-z On the other hand, past observations suggest enhanced bolometric luminosity of QSOs relative to the case of the parallel growth, or, star formation (FIR) luminosity is lower. this can also be checked with our new measurements! (differential- Willott, Omont, & Bergeron z 6 quasars. Magorrian Symbols as for Figurerelation) 6. The black line with gray shading is the local galaxies with the lowest L FIR at a given L Bol are expected to have a significant fraction of their L FIR due to quasar-heated dust (Netzer et al. 2007). correlation 1s scatter from the work of Kormendy & Ho (2013) equating M dyn to M bulge. The CFHQS quasars lie on the local relationship and do not show the large offset displayed by the most massive black holes. Uncertainties Figure in M dyn have 2 shows not been previously calculated due published to the reasons datagiven for individually the text. detected Does z 6AGN-feedback quasars and stacked averagesinhibit from WangSF? et al. (2011a) andomontetal(2013). Thedottedlineisthe relationship Does between LFIR L FIR and fail L Bol to foundtrace by Wang etsf al. (2011a) effectively for stack averages of quasars at 2 <z<7. Note that both the stacked due averages to andlower the relationship dust from Wang content? et al. (2011a) have been renormalized according to bolometric correction adopted Discriminating here (see Omont et al. 2013 these for moreis details). very Gray important crosses are a complete sample of low-redshift (z <0.5) optically selected topic Palomar Green for ALMA (PG) quasars observations. (Hao et al. 2005). L FIR for PG quasars has been estimated as 2 luminosity at 60 µm - we may need other tracers of SFR (Lawrence et al. 1989). Note that many of the highest luminosity (most distant) quasars in the PG sample are undetected at 60 µm and only have upper limits on L FIR. As noted by Wang et al. (2011a), the z 6stackedaverageslieclosetothecorrelation exhibited by low-redshift quasars, indicating no enhancement in SFR at high redshift for a given quasar luminosity. 5
MBH [Msun] z ~ 6 or higher Science Case (2) Co-evolution at high-z We should also recall there may exist a selection bias preferring luminous (= massive) QSOs. previous studies can be biased toward high-mbh direction Willott et al. 2015, ApJ, 801, 123 σ [km/s] The Astrophysical Journal, 770:13(7pp),2013June10 LFIR [Lsun] Willott et al. 2013, ApJ, 770, 13 LBol [Lsun] Figure 2. Far-infrared luminosity vs. AGN bolometric luminosity for z 6 quasars. The two CFHQS quasars observed with ALMA in this paper are shown Theoretical models predict there is little Willott, Omont, & Bergeron z 6 bias quasars. Symbols for asmbh for Figure~ 6. The 1e8 black line Msun with grayobjects shading is the local(e.g., galaxies correlation with 1the s scatter lowest froml the FIR work at a of given Kormendy L Bol are & Ho expected (2013) equating to have Lauer M dyn a to significant M bulge. et Thefraction CFHQS al. 2007, quasars of their lie on L FIR ApJ, thedue localtorelationship 670, quasar-heated and 249). do not dust (Netzer et al. 2007). Figure 2 shows previously published data for individually detected z 6 quasars and stacked averages from Wang show the large offset displayed by the most massive black holes. Uncertainties in M dyn have not been calculated due to the reasons given in the text. et al. (2011a) andomontetal(2013). Thedottedlineisthe Going to less-luminous objects (HSC!!) relationship between L FIR and L Bol found by Wang et al. (2011a) for stack averages of quasars at 2 <z<7. Note that both the and measuring the scatter of each stacked averages and the relationship from Wang et al. (2011a) have MBH-bin been renormalized will according give to the us bolometric a hint correction on this adopted here (see Omont et al. 2013 for more details). Gray crosses problem. are a complete sample of low-redshift (z <0.5) optically selected Palomar Green (PG) quasars (Hao et al. 2005). L FIR for PG quasars Beautiful has been estimated collaboration as 2 the luminosity at 60 of µmhsc with (Lawrence et al. 1989). Note that many of the highest luminosity (most ALMA distant) quasars in the PG sample are undetected at 60 µm and only have upper limits on L FIR. As noted by Wang et al. (2011a), the z 6stackedaverageslieclosetothecorrelation exhibited by low-redshift quasars, indicating no enhancement in SFR at high redshift for a given quasar luminosity. 6
Science Case (3) AGN feedback as gas outflows multiple-outflow? Cicone et al. 2015, A&A, 574, 14 Recently, an extended (~30 kpc) massive cold gas outflow of a few 100 Msun/yr was found in J1148+5251 at z = 6.4! Detecting the rather faint wing component requires a quite high sensitivity and a wide bandwidth ALMA! 7
Sub-kpc imaging of bright quasar host galaxies at z~7 B. Venemans, F. Walter, R. Decarli, L. Zschaechner, E. Banados, and E. P. Farina; accepted for ALMA Cycle 3 High redshift quasars are likely hosted by massive and luminous galaxies in the early universe. Recently we discovered several bright quasars at 6.5<z<7.1, providing a unique opportunity to study the physical properties of massive galaxies at z~7. Our ALMA Cycle 1 and PdBI data of 5 of these sources already revealed strong [CII] emission and far-infrared (FIR) continua. These are the only objects currently known at z>6.5 with bright [CII] emission. Here we propose to obtain followup observations of this small sample at sub-kpc resolution (0.7 kpc or ~0.12") to, for the first time, address key aspects that cannot be answered with the available data: Utilising the unique capabilities of ALMA, we will be able to (1) constrain the morphology and kinematics of the emission line gas, (2) produce a map of the star formation as traced by the FIR, (3) look for possible recent merger events, (4) search for infall/outflow signatures and (5) derive a well-constrained dynamical mass. Observations of this small sample will thus greatly enhance our knowledge of and provide first statistics on the properties of the earliest massive galaxies when the universe was only ~800 Myr old. 8
After that (i.e., cycle 5 or later) CO SLED No strong difference from local ones Wang et al. 2010, ApJ, 714, 699 Nagao et al. 2012, A&A, 542, L34 We will continue to observe other lines such as multi-transition CO, other fine structure lines such as [NII]. constrain gas excitation conditions; metallicity measurements of QSO-host galaxies Going to higher resolution is of course a choice. 9
After that (i.e., cycle 5 or later) [CII] J0365+0305 z=6.53 H2O(!?) High abundance of water vapour could exist in galaxies with extremely low metallicity (1e-3 solar) expected for the first generation of galaxies!! Banados et al. 2015, ApJ, 805, L8 Does this indicate high metal around the AGN, but low metal in its host? Correct interpretation of H2O requires multi-transition analysis of this molecule. 10