MApping the Most Massive Overdensity Through Hydrogen (MAMMOTH) Zheng Cai (UCSC)

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1 MApping the Most Massive Overdensity Through Hydrogen (MAMMOTH) Zheng Cai (UCSC) IGM Conference From Wall to Web, Berlin, 2016

2 IGM tomography (Lee+ 14, 15, 16; Stark+ 15ab): IGM Tomography a reconstruction of the 3D Lyman alpha forest absorption, revealing cosmic webs on Mpc scales. This technique has a high completeness in searching for protoclusters. We (Cai et al. 2015, 2016ab in prep.) present that the SDSS-III/BOSS data can already be used to search for large-scale structures associated with highest overdensities.

3 Why overdensities are important 1 Abundance and mass provide sensitive constraints to Cosmology and cosmic structure formation (long-term goal) Log N Mortonson, Hu, Huterer 2011

4 2 High-z overdensities provide unique laboratories for studying galaxy formation Big questions: when the galaxies start to quench? Why overdensities are important Do galaxy properties depend on their environments at z=2-3? emergence color/density morphology relations? Figure from Newman et al. (2014): majority of galaxies in overdensities at z=1.6 are quenched. How about z>2?

5 Why overdensities are important 3 galaxy-igm interaction in protoclusters Big questions: e.g., What drives the intense star formation? accretion from filaments or mergers? (Caesy et al. 2016) Lee et al. (2014)

6 Traditional ways of tracing high-z matter overdensities: 1 Use biased halos, such as QSOs/radio galaxies, small duty cycles. Selection incomplete. 2 Galaxy redshift survey (e.g., Steidel et al. 1998): survey volumes are often limited

7 Lyman alpha absorption tracing underlying matter overdensities Matter Overdensity Peirani et al. (2014) Position (Mpc/h) Large scale overdensity à large EW of absorption Transmitted Flux in QSO spectra Coherently strong Lya absorption (CoSLAs) Cai et al. (2015)

8 Lyman alpha absorption tracing matter overdensities! SDSS/BOSS+ eboss and future surveys (Pieri s talk) provide quasar spectroscopy over a large sky coverage at z > 2. BOSS/e-BOSS Data Release has obtained > 200,000 quasar spectra over 10,000 deg2 Assuming each QSO 500Mpc, survey volume > 5 Gpc3

9 Lyman alpha absorption tracing underlying matter overdensity Mukae et al., including Cai (2016)

10 Cosmological Simulations Peirani et al. (2014) LyMAS Simulation (1.0h 1 Gpc) particles Cross-correlation of e Mass

11 Tracing large-scale (20 Mpc) overdensity using different methods Most of the systems traced by strong Lya absorption represent 0.5% of the most massive overdensities. Cai et al. (2015)

12 Example of Lya absorption tracing matter overdensity at z=2.5 Coherently strong Lya absorption (CoSLAs) traces filamentary structure on 20h 1 Mpc Cai et al. 2015

13 Lyα absorption around confirmed overdensity SSA22 overdensity at z=3.1 (Steidel et al. 1998, 2000) SDSS-III/BOSS spectra

14 Selection of the coherently strong Lya absorption Cai et al. 2015

15 an example of DLA contaminant Cai et al. 2015

16 Examples of CoSLA candidates at z=3 Cai et al Lower right is the BOSS spectrum. Black is Ly-alpha, blue is Ly-beta

17 Examples of CoSLA candidates at z=3

18 20 h -1 Mpc IGM absorption + multi-quasars within 30 Mpc at z=2.32+/-0.02

19 15Mpc Cai et al. (2016a) ready to submit

20 Examples of spectroscopic confirmed LAEs f (erg s 1 cm 2 Å 1 ) Cai et al. (2016) ready to submit

21 Working in Progress 1 Keck 2 night LRIS, have spectroscopy of 100 galaxies in this field down to 0.5 L*, fully map the 3D structures in this field. Data quality may good for an initial tomographic study. 2 HST/WFC3 program (cycle 24, PI: Cai) and use 10 mosaic pointings to map the field. -- examine the environmental dependence of galaxy properties at z= check whether merger or accretion from cosmic webs power intense star formation, by combining the tomographic map and HST imaging. 3 UKIRT/WFCAM infrared imaging, already finished a 20-hour imaging in J, H, K. -- follow-up MOSFIRE -> the quenching fraction -- galaxy stellar mass function in the protocluster.

22

23 One ultraluminous Lyman alpha blob/nebula 100 kpc 100 kpc

24 Size - luminosity of various Lya nebula Cai et al. 2016b in prep. Also see Cantalupo et al. 2014

25 AGN photoionization scenario Cai et al. 2016b in prep. Also see Arrigoni-Batta et al. 2015ab Our observed SB CIV = 1 x erg s -1 cm -2 arcsec -2.

26 AGN photoionization scenario =1 Cai et al. 2016b in prep. Our observed SB CIV = 1 x erg s -1 cm -2 arcsec -2. Note N CIV is <~10 14 cm -2 (Lau et al. 2015). N CV <~10 14 cm -2 for plausible ionization parameters. f C ~0.05, n H ~ 500 cm -3 then there is a reasonable N CV à a low covering factor, high density gas phase existed in QSO halos.

27 CWI/KCWI to fully map kinematics and morphology of LABs. Collaborate with Hamden and Martin Martin et al Matuszewski et al. (2011)

28 Summary Large-scale structure is important for both studying cosmology and galaxy/igm interaction. Strongest intergalactic Lyman alpha absorption (group) can be a very effective way to trace extreme overdensities/proto-clusters from huge survey volume. We systematically select pilot fields at z=2.3 from Gpc 3 survey volume. A more efficient way of searching Lyman alpha nebulae. Further surveys from complete SDSS-IV, DESI, PFS will select more extreme systems to constrain cosmic structure formation, galaxy evolution and the IGM-galaxy.

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