Panoramic mapping most massive HI structures & connecting ISM, CGM, and IGM at cosmic noon Rhythm Shimakawa (SOKENDAI/JSPS/NAOJ UCO/Lick (UCSC)) NAOJ: N. Kashikawa, T. Kodama, I. Tanaka, Y. Matsuda, et al. UCO/Lick (UCSC): J. X. Prochaska, Z. Cai, et al. WS (Jan. 2017) Rhythm Shimakawa 1
Massive HI structures & connecting ISM CGM IGM Subaru, Keck z=2-3,, ISM-CGM-IGM Subaru Keck 20 ( ) PFS-SSP PFS-SSP conflict PFS-SSP IGM tomography Subaru, Keck win-win UC (Santa Cruz) flexible WS (Jan. 2017) Rhythm Shimakawa 2
Galaxy diversity vs environments Downloaded from http://mnras.oxfordjournals.org/ at National AstronomicalObservatory, Japan on February 3, 2016 Seek for causal physical origins galaxy diversity triggered by environments spiral fast slow Morphology density relation Cappellari et al. 2011 Figure 8. The T! relation for fast rotators (blue ellipse with vertical すばる ケック連携のための WS (Jan. 2017) Rhythm Shimakawa 3
Massive starbursts in a z 2 proto-cluster Galaxy formation in protocluster core Figure 6. Close-up views USS 1558-003 radio galaxy at z = 2.53 in NB2315, Ks, and NB2315 Ks images. Note that FWHM values PSF in se Ks and NB2315 images 0. 40 and 0. 36, respectively, since se images created by combining only frames taken under excellent seeing conditions 0. 4. The length bar in NB2315 Ks image indicates angular size 4. 5, which corresponds to 36.2 kpc in physical scale. The NB2315 Ks image clearly indicates that radio galaxy has an extremely extended Hα emission. 4.2. Color Magnitude Diagram First appearance red sequence in protocluster core The color magnitude diagram is a powerful tool for investigating properties galaxies in clusters or proto-clusters. It is well known that galaxy clusters at low redshifts dominated by quiescent galaxies which make up red sequence on color magnitude diagram. The tight sequence red galaxies is one prominent features seen in galaxy clusters. However, when and how do such red quiescent galaxies form and evolve? The answer to this question still remains unclear, although re is some evidence suggesting that blue star-forming galaxies in early universe evolve and become red quiescent galaxies in high density regions during redshift interval 2 3 (e.g., Kajisawa et al. 2006a; Kodama et al. 2007; Kriek et al. 2008; Doherty et al. 2010; Gobat et al. 2011). To address this, it is essential to investigate furr color magnitude diagram for galaxy cluster and proto-cluster at high redshifts when clusters vigorously evolving. Figure 7 shows a color magnitude diagram J Ks versus Ks for galaxies in observed field 4. toward proto-cluster Figure Left: 2D map Hα emitters around PKS 1138. The black squs show Hα emitters which satisfy BzK selection, while black c USS 1558-003. The HAEs associated with proto-cluster Hα emitters which do not satisfy BzK selection. The triangles show Ks -undetected emitters. The red filled circles and black open squs s plotted by open circles. As presented by Kodama et al. and X-ray-detected emitters, (2007), we may be able to recognize a sequence DRGs at respectively. Grey points show all NB2071-selected sources, and DRGs marked with red open circles. Note that Figure 7. Color magnitude diagram J Ks vs. Ks. The blue open circles Herschel protocluster survey J Ks 1.5, which corresponds to color quiescent Hα emitters z = 2.53, dots BzK show allinformation galaxies in below this line. The coordinates given relative to central ra data only available at "Dec.show 3.5, soatthat we and do notblack have galaxies with formation redshift 3! zf < 4 (Kodama observed field. The long-dashed, short-dashed, and dotted lines show 5σ, 3σ, large grey circle shows masked due to some bright sources. line at "Dec. = 2.0 shows dividing line high- and 2σ limitsregion in color and magnitude. The red solid horizontal line The shows dotted et al. 1998), as indicated by The tickmarks in figure. It is and color corresponding to J K = 1.38, which is a criterion for selecting DRGs. s not surprising that majority HAEs used located environments in thisonpaper.theright: (J Ks ) versus Ks colour magnitude diagram for high-density proto-cluster and low-density galaxies with formation redshifts zf J Ks colors red quiescent bluer side diagram. However, it is intriguing that = 3, 4, and 5 shown by tickmarks at left edge, which estimated greysatisfying dots indicate NB-selected sources, and black squs Hα emitters (red filled circles for MIPS-detected emitters). The diam some HAEs have very red colors DRGall criterion by Kodama et al. (1998) model. The dotted curves show isostellar mass and constitute mainly faint end panel red sequence. bottom z =We 2.2 Hαcurves emitters in11 GOODS-N field. The vertical and slanted dashed lines show 3σ and 2σ limiting magnitudes Ks for 1 10 M and 1 1010 M, respectively. also note that re is a significant color scatter among red (A color version this figure is available in online data, respectively. The locations red sequence in case zjournal.) f = 3, 5, 10 modelled by Kodama & Arimoto (1997) shown as dotted li HAEs. Similarly, red HAEs and dusty star-forming galaxies 11 M ) based on model Kodama et al. (1999). The colour distribution dash dotted line shows line around (corresponding to 10 have also been recognized by Figure recent observations clusters at iso-stellar-mass squs show Hα emitters which satisfy BzK selection, while black c 4. Left: 2D map Hα emitters PKS 1138. The black lower redshifts (Geach et al. 2006; Koyama et al. 2010, 2011). HAEs based on ir Ks -band magnitudes and J colour Ks definitions. within each environment is shown as histogram, where we also show our Hα emitters which do not satisfy BzK selection. The triangles show K -undetected emitters. The red filled circles and black open squs s They tend to be dusty star-forming galaxies and considered colors. The relationship between J Ks colors and M /Ls Ks is to be in transition phase from active star-forming galaxies to and X-ray-detected emitters, respectively. Grey points show population NB2071-selected approximately estimated using all stellar synsis sources, and DRGs marked with red open circles. Note that passive quiescent galaxies, probably under influence some model Kodama et we al. (1998, 1999), where we constructed abelow this line. The coordinates given relative to central ra data only available at "Dec. 3.5, so that do not have BzK information environmental effects, becausewhere se star-forming preferentially found in sequence models with varying bulge-to-disk We note selection technique and all broad-band filters used in populations also due highly clustered inratios. The The large grey atcircle shows here masked region to some bright sources. dotted line at "Dec. = 2.0 shows dividing line high- and medium density regions galaxy clusters intermediate that because SED degeneracy among age, metallicity, exactly same as those used in this After ap proto-cluster core (see consistent results from 1.5! z! 2.5 cluster redshifts (z! 0.8) when andenvironments where we see a sharp transition dust extinction, J Ks and used in this paper.andright: (J Ks )relationship versus Ksbetween colour magnitude diagram for high-density proto-cluster andstudy. low-density in distribution galaxy colors from blue to red (Tanaka M /L insensitive to detailed modeling same flux and EW cut, we add se sources in our fie Ks is relatively studies Hayashi al. 2010; Hilton et al. and 2010; Tran et al. 2010). grey dotsbyindicate all et sources, black Hα emitters (red filled circles for MIPS-detected emitters). The diam et al. 2005; Koyama et al. 2008). Therefore, it is suggested thatnb-selected stellar populations except for effect squs initial mass function faint end red sequence is just being built those sample. Neverless, structure 1138 is also suggested bottom panel by z= 2.2 Hαaround emitters in PKS field. The(1955) vertical and dashed lines show 3σ and 2σ limiting magnitudes Ks (IMF) variation. WeGOODS-N here assume Salpeter IMF, andslanted transitional galaxies recognized as red HAEs. stellar masses in models scaled accordingly. From data, locationsred red sequence in zf = 10 modelled by Kodama Arimoto (1997) shown as Hα dotted li In Fig. 4, we &find a large number red emit an analysisthe distant galaxies (DRGs) by case Kodama et 3,al.5,between For a galaxy at z = 2.53,from its Krespectively. s -band luminosity is still this experiment, we establish following relationship 11 a good proxy for stellar(2007), mass. However, mass-todash dotted line shows iso-stellar-mass linehα (corresponding M ) based(jon Kodama et al. (1999). They colour distribution stellar mass (M andpresented J tok10 some extreme cases, satisfy D Kmodel although structure traced by emitters ), K s magnitude, s color:in s ) " 1.In luminosity ratio (M /LKs ) is dependent on SED, and it should within each environment shownmore as histogram, This wheremay we also show our colourtion definitions. criteria with (J Ks ) > 1.38 [equivalently, (J K this study appears tos -band beismuch prominent. be because be corrected to get a more precise stellar mass from K 11 log (M /10 M ) = 0.4(K K ) + log M, (4) luminosity. We use a simple method to estimate stellar masses s 11 10 10 2.3]. We confirmed that two red sources with Hα DRG selection picks up distant galaxies over a wide range c.f. Kodama+07, Hayashi+12, Koyama+13 Rapid declining star-forming activities in protocluster core z=2.53 2.15 Hayashi+12, Koyama+13 6 z) + 1 ( 7 c.f. Clements+14, Smail+14, Shimakawa+14, Kato+16 shown in technique spectroscopic study by Doherty et al. (2010 selection and all broad-band filters used in selected as red emitters in this study. Importantly, we find exactly same as those used in this study. After ap red Hαflux emitters cut, predominantly found in in proto-clu same and EW we add se sources our fie ronment, while y very r in low-density envir sample. Kolmogorov Smirnov shows that probabili In Fig. 4, we find a(ks) largetestnumber red Hα emit colour distribution highand low-density samples satisfy D (J Ks ) " 1. In some extreme cases, y (2007), although structure traced by Hα emitters presented in Kato+16 from same pnt population is only 0.1 per cent. 1.38 [equivalently, (Jhigher We K tion criteria with (J Kour this study appears to be Figure much5.more prominent. This may be because 3 104 times s) > SFR density clusters, protoclusters, and global cosmic SFR densities. The SFR densities protoclusters 10 4.2 Red star-forming galaxies and ir environment this result may partly be produced by presence X-ra 2.3]. We confirmed thatand sources with4which Hα DRG selection picks galaxies over 2014). a wide range globalup SFRdistant density (Madau & Dickinson We show compilation from Dannerbauer et al. (2014) datatwo from red Clements et al. (2014), すばる ケック連携のための WS (Jan. 2017) Rhythm Shimakawa in redshift (e.g. Franx et7 al. 2003), diluting clustered contrast where star-forming populations also highly in any structures. We check spatial distribution DRGs throughout proto-cluster core (see consistent results from 1.5! z! 2.5 cluster fieldby(fig. 4) and et spatial distribution 2010). DRGs studies Hayashi et confirm al. 2010;that Hilton al. 2010; Tran et al. is qualitatively consistent that PKS Hα emitters, but again, Neverless, structurewith around 1138 is also suggested structure looks less from an analysis prominent. distant red galaxies (DRGs) by Kodama et al.
CGM in protocluster core Cold streams penetrate through hot media especially critical for z>2 massive structures CGM controls mass and gas assembly, and subsequent SF activities Dekel+2009a,b Coma (Chiang+14) c.f. Dekel+09a,b, van de Voort+12 WS (Jan. 2017) Rhythm Shimakawa 5
Mass and SFR enhancements in protocluster core MAHALO-DEEP survey (MOIRCS 10hrs for USS1558 at z=2.5) 100 150 200 hai 5th [ph-kpc] 0.5 Dec. [ph-mpc] 0.0-0.5 - -1.5-2.0 0.5 0.0-0.5 - R.A. [ph-mpc] Hayashi+16; Shimakawa+in prep. WS (Jan. 2017) Rhythm Shimakawa 6
LAE deficiency in protocluster core First direct evidence Lyα depletion in protocluster cores due to higher HI covering fractions? Dec. [deg] -0.2-0.3-0.4-0.5-0.6 0 1 2 3 4 [ ] Cumulative number 0.5 0.0 LAEs HAEs 1% 11% lower density 0 100 200 300 400 hai 5th [ph-kpc] 10 co-mpc Dec. [ph-mpc] 0.5 0.0-0.5 - -1.5-2.0 100 150 200 hai 5th [ph-kpc] 30 diameter 240.6 240.5 240.4 240.3 R.A. [deg] 240.2 240.1 0.5 0.0-0.5 - R.A. [ph-mpc] Shimakawa et al. submitted WS (Jan. 2017) Rhythm Shimakawa 7
Science motivation CGM z<2.6 (HAEs) vs. z>2.6 (LAEs) (, z ) PFS-SSP: 15 deg 2, 30 fiber separation CGM, SFR, ISM, etc CGM, HI, covering fraction, etc WS (Jan. 2017) Rhythm Shimakawa 9
6 16 Coherently strong intergalactic Lyα absorption systems Mass in 15 h 1 TABLE 1 Mpc cubes centered on different objects Cai et al. 2016 Lyα (LAF) analyses length forest specific absorption system. Themass airmass Center Median 15h 1 Mpc (1014 M ) observations were about 1.4, (and we used M2 ) positions >> 15 PFS angles close to parallactic angle. Spectrophotometric standard and Random stars were observed for 2.6flux calibration, 1.2 12 Mfor a CuAr arc was 10 used calibration. Quasars (Mlamp ) wavelength 3.7 1.6 halo = 2-3 13 Mhalo a typical 5 10 CNR M 6.110 in absorption We Halos havewith reached CoSLA (no noise) 7.0 1.6 3 region. 6 4 2 0 4550 4600 4650 4700 4750 4800 Wavelength (Å) 4850 4900 Mpc 1.5 0.5 0.0 30 20 10 0 10 20 1 Comoving Distance ( h Mpc) 30 1.5 Ly α Ly β DLA Ly α Data Ly α 1.5 Fig. 6. The cumulativedla probability mass within (15β h 1 Ly β Data Ly Mpc)3. The x-axis is mass within (15 h 1 Mpc)3 cubes. The 0.6 y-axis is cumulative probability. Yellow shaded a shows mass distribution (±1- ) traced by quasar halos. Purple shaded a represents mass distribution centered at most massive halos 0.0 0.6 in LyMAS simulation (Mhalo > 1013.7 M ). The red shaded 1 Mpc a represents mass traced 30 20 10 by 0 CoSLAs 10 on 15 20 h 30 1 scale, selected spectra. 0.0 from noise-added Comoving Distance ( h Mpc) Transmitted FluxFlux Transmitted low shaded a) well satisfies selection criteria CoSLAs on 15 h 1 Mpc centered at 4755 A (z = 2.91). From BOSS data, e ective optical depth this system is e = 1.61+0.10 0.10, a factor 4.8 mean optical depth at z = 2.91. The middle panel presents e ective optical depth 15h 1 Mpc on 15 h 1 Mpc ( e ), greater than our selection threshold (blue horizontal line) 4.5 h e i. The lower panel presents MMT follow-up observations this target with 3 30 min exposures using 1200 lines mm 1 grating. With MMT spectra, we can resolve any Ly and Ly absorbers with rest-frame Doppler parameter b > 100/(1 + z) = 25 km s 1. From lower left panel, EW ratio between Ly (blue) EWLy and Ly (black) is EWLy = 0.88+0.03 0.03, which suggests that this absorption consists superposition a series individual absorbers with NHI 1015 18 cm 2 (Figure 15).The This absorption system Fig. 5. distribution mass traced is by similar di erent to objects. strongest intergalactic Ly (15 absorption LyThe x-axis is mass within h 1 Mpc)3predicted cubes. Theiny-axis J025252.07+025704.0 2.0 1 CoSLA = 4σ excess in τ over co-mpc along LOS From 15 BOSS spectrum, this absorption system (yel- τ15h eff Note. Summary mass within 15 h 1 using di erent trac6.2.1. J025252.07+025704.0 ers in LyMAS simulation. HI (no noise) represents mass traced opttarget. Figure 20 selected presents spectra, this by CoSLAs from spectrum original mock no noisethe being added; CNR=4 mass traced by strongest upper panelcosla presents shows SDSS-III/BOSS spectrum. absorption selected from noise-added spectra. fλ(10 17 erg s 1 cm 2 Å 1) SDSS/BOSS-III (10k deg ) 160,000 LAF spectra QSOs Effective CoSLA CNR=4volume size 6.7 ~ 1 co-gpc 1.6 1014-3020. 0 distribution 30 CoSLAs have a -20 comparable mass those Fig. The -10spectra -110CoSLA20 tocandidate Distancepanel Mpc) J025252.07+025704.0. The upper shows centered on most Comoving massive single (hhalos with M > haloboss 13.7 spectrum, with absorption marked in yellow shadedmore a. than Orange 10 M (purple dot-dashed histogram). Fig. 21. A comparison between CoSLA candidate shows continuum using mean optical depth regulated PCA half CoSLAs top 0.2%LLS) most すばる ケック連携のための WSamiddel (Jan. 2017) Rhythm Shimakawa 10 15 J025252.07+025704.0 and sub-dla (super NHI = fit (Lee et al. 2012). represent The panel presents with massive over
Pair filters at z=2.15 2.20 and 3.30 3.35 HSC (Lyα) MOIRCS (Hα) 1. HSC - LAEs: ( ) PFS SDSS/BOSS HI 2. MOIRCS - HAEs: CGM, 3. MOSFIRE (Keck): ISM (Z, U, Ne, A Hα ), z 4. LRIS & KCWI (Keck): CGM (Z, N H I, f H I) Transmittance 0.8 0.6 0.4 0.2 Transmittance 0.8 0.6 0.4 0.2 2.15 2.20 H redshift NB2085 NB387-w z=3-4 z=2-3 BrG NB527-w z=1-2 z=0 3.25 3.30 3.35 3.40 [OIII]redshift WS (Jan. 2017) Rhythm Shimakawa 11
The most massive HI structures An example: most massive HI structure at z=2.3 5 QSO sight lines in background, 6 QSOs associated x11 denser than random fields An enormous Lyα blob associated with structure 5 40.4 Strong Lyα Absorption Lyα emitters 10 h 1 galaxies at z=2.306-2.330 BOSS Quasars at z=2.306-2.319 galaxies at z=2.319-2.330 BOSS Quasars at z=2.319-2.330 cmpc 6 Cai et al. arxiv-a,b 40.2 DEC DEC (Degree) Enormous Lya Nebula N$ E$ 40.0 Source B! 39.8 53 $ 220.6 220.4 220.2 220.0 RA (Degree) RA. 6. The galaxy overdensity BOSS1441 at z = 2.32 ± 0.02, selected from SDSS-III/BOSS DR9 database. This structure is traced group Ly absorption systems (orange diamonds) and QSOs (brown asterisks) over 30 h 1 cmpc at z = 2.3. すばる ケック連携のための Each Coherently WS (Jan. image 2017) Fig. 2. Continuum-subtracted, smood narrow-band g Ly Absorption (CoSLA) candidate is presented in Figure 2 and Figure 3. Our LBT/MODS spectroscopy have targeted 20 LAEs Rhythm Shimakawa 12 field around enormous Ly nebula (ELAN) M
Team, win-win situation HSC+MOIRCS(+PFS) MOSFIRE+LRIS+KCWI Young users Subaru & Keck! R. Shimakawa Z. Cai N. Kashikawa J.X. Prochaska T. Kodama I. Tanaka Y. Matsuda R. Shimakawa Lyα, Hα line mapping LSSs, Protoclusters, cores LABs and members Opt+NIR spectroscopy SF, AGN activities ISM, CGM properties WS (Jan. 2017) Rhythm Shimakawa 14
Wish list 1. PFS-SSP or S17B,18A 2. 3. SSP 4. PFS-SSP conflict PFS-SSP 5. PFS-SSP WS (Jan. 2017) Rhythm Shimakawa 15
1. Subaru-PFS-SSP Keck 2. Subaru- Keck PFS-SSP SSP SSP win-win WS (Jan. 2017) Rhythm Shimakawa 16