Diffuse Media Science with BigBOSS

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Marilynn Wilkinson
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1 Diffuse Media Science with BigBOSS J. Xavier Prochaska Interstellar Medium Program of Studies (IMPS) UCO/Lick Observatory UC Santa Cruz 1

2 Diffuse Media My (loose) definition: n H < 1 cm -3 Intergalactic Medium (IGM; >>1 Mpc) Intracluster Medium (ICM; ~1Mpc) Circumgalactic Medium (CGM; ~100kpc) Ambient Interstellar Medium (ISM; 10kpc) }>99% of the volume >90% of z~0 baryons Constituents Gas, metals, dust Neutral and ionized gas Accreting and outflowing material 2

Diffuse Media My (loose) definition: n H < 1 cm -3 Intergalactic Medium (IGM; >>1 Mpc) Intracluster Medium (ICM; ~1Mpc) Circumgalactic Medium (CGM; ~100kpc) Ambient Interstellar Medium (ISM; 10kpc)

3 Diffuse Media My (loose) definition: n H < 1 cm -3 Intergalactic Medium (IGM; >>1 Mpc) Intracluster Medium (ICM; ~1Mpc) Circumgalactic Medium (CGM; ~100kpc) Ambient Interstellar Medium (ISM; 10kpc) }>99% of the volume >90% of z~0 baryons Constituents Gas, metals, dust Neutral and ionized gas Accreting and outflowing material The Diffuse Medium has too low density to be detected in emission beyond the local universe. Absorption is King+Queen 2

4 Science with Diffuse Media Cosmology BAO Power spectrum Non-gaussianity Baryonic Census Gas, metals, dust Characterizing the IBL McDonald+06 3

5 Science with Diffuse Media Galaxy Formation ISM dynamics Chemical evolution Gas accretion Feedback processes Energy, gas, metals Mergers (tidal debris) Relative Flux Weiner+09 [OII] MgII!1500!1000! Relative Velocity (km s!1 ) 4

6 Prochaska+03 Science with Diffuse Media Star Formation Formation of H2 Dust depletion Nucleosynthetic yields 5

7 Science with Diffuse Media Kanekar+10 Fundamental Physics Evolution of the physical constants Neutrino mass 6

8 DM: Lessons from SDSS (Focus on the Quasar Spectroscopy of SDSS) Advantages Sample size Spectrophotometry Disadvantages Spectral resolution Limited blue coverage Higher density of UV transitions at higher energies 7

9 SDSS: Absorber Surveys Damped Lya Systems (ISM) MgII Systems (ISM/CGM) 100,000 quasars Semi-automated searches Human vetting was tractable Spectrophotometry not essential 8

SDSS: Absorber Surveys Damped Lya Systems (ISM) MgII Systems (ISM/CGM) 1.4! HI (10 8 M Sun Mpc!3 h 72 ) 1.2 1.0 0.8 0.6 0.4 0.2 0.0 2.0 2.5 3.0 3.5 4.0 4.5 5.

10 SDSS: Absorber Surveys Damped Lya Systems (ISM) MgII Systems (ISM/CGM) 1.4! HI (10 8 M Sun Mpc!3 h 72 ) z Prochaska+09 Nestor+05 Primary science (from counting absorbers) Limited by systematics (e.g. dust), not statistics Additional sample size may have limited value Mainly comes for free in the main survey 9

11 SDSS: Needles in the Haystack Damped Lya Systems (ISM) MgII Systems (ISM/CGM) Nestor+10 Tails of the distributions In metallicity, kinematics, HI, dust content, etc. Rarer than 1/100 Push physical processes to their limits 10

SDSS: Needles in the Haystack Quasar/Quasar Pairs Quasar/Galaxy Pairs Prochaska U086 2012A Proposal Q Hennawi+06 Arcseconds 0 0 Fig. 1.

d 10 the J2049-0012 quasar/galaxy system (z = 0.36 H! [OIII]"" 4959, 5007 60 Keck/LRIS 600/7500 grating.

The bright quasar Observed Wavelength [Å] Rare configurations Physical or projected Sensitive probes of kpc scales (CGM) Target selection

12 SDSS: Needles in the Haystack Quasar/Quasar Pairs Quasar/Galaxy Pairs Prochaska U A Proposal Q Hennawi+06 Arcseconds 0 0 Fig. 1. (left) SDSS 5 color image of the qua 5 Note how the stellar distributions in 20 this image while the the spectrum clearly presents 40tidal d 10 the J quasar/galaxy system (z = 0.36 H! [OIII]"" 4959, Keck/LRIS 600/7500 grating. The continuum lig horizontal 6800 bands in the6850 image. The bright quasar Observed Wavelength [Å] Rare configurations Physical or projected Sensitive probes of kpc scales (CGM) Target selection critical Arcseconds dasilva+10 Chen+10 0 Tumlinson h 1 kpc 11 H! saturates the image in this stretch. These emissio companion galaxy as well as a bridge of emissio both galaxies (see Fig. 3). The emission lines are

13 SDSS: Smoothing the Samples Stacked spectra (Absorber frame) Pieri+10 Great for visualization of absorption lines Spectrophotometry not essential Limited physical measurement 12

14 SDSS: Smoothing the Samples Stacked spectra (Absorber frame) Menard+10 York+06 Dust extinction Map diffuse dust to tens of kpc Extinction law (SMC) Spectrophotometry (and photometry) critical 13

15 SDSS: Smoothing the Samples Stacked spectra (Absorber frame) Menard+11 Coincident [OII] emission Spectrophotometry critical Cosmological SFR density from diffuse gas tracer 14

SDSS: Smoothing the Samples 0.6 0.4 Stacked spectra (Quasar frame) 1.5 f /f 912 1.0 0.8 0.6 0.4 0.2 Prochaska+09 log[f! /f 1450 ] 0.2 0.0 f /f 1450 1.0 0.5 0.

16 SDSS: Smoothing the Samples Stacked spectra (Quasar frame) 1.5 f /f Prochaska+09 log[f! /f 1450 ] f /f rest Ly Ly! Ly!0.4 Suzuki ! rest (Angstroms) rest [1+z q ] (Angstroms) Average IGM opacity Lya forest (DA) Mean free path

SDSS: Smoothing the Samples Stacked spectra (SF galaxies) = Chen+10 Normalized flux 1.5 1.0 0.5 0.0 0.5 1.2 1.1 1.0 0.9 0.8 5050 5100 5150 5200 5250 5300 4000 4500 5000 5500 6000 6500 1.2 1.1 1.0 0.9 Wavelength (Å) 0.

17 SDSS: Smoothing the Samples Stacked spectra (SF galaxies) = Chen+10 Normalized flux Wavelength (Å) Wavele Search for Galactic-scale winds Offset NaI absorption Correlate with galaxy properties (e.g. inclination) Continuum normalized spectrum i=[0, 10] i=[20, 30] i=[40, 50] i=[60, 70] 16

measure column densities Physical quantity R=5,000 is tantalizing Would require very high S/N (>20)

18 BigBOSS Requirements: Diffuse Media (My) Technical requirements; not targeting Signal-to-noise >5 for individual absorbers Wavelength coverage Bluer is better; nuff said Spectral resolution R=3,000 is too low to faithfully measure column densities Physical quantity R=5,000 is tantalizing Would require very high S/N (>20) Spectrophotometry Critical to smoothing experiments Relative more than absolute Can high precision be achieved with 1.5 fibers? 17

HI Reionization at z>6 HeII reionization at z~3, too Extent/Mass/Energy of Feedback SF-driven

19 Open Science Topics/Questions in DM Some of which lie beyond BigBOSS Enrichment of the z<1 IGM Do metals extend beyond the CGM? HI Reionization at z>6 HeII reionization at z~3, too Extent/Mass/Energy of Feedback SF-driven (SNe, radiation) Quasar-driven WHIM or not a WHIM? Thermal history of the IGM Blazars?! Dust beyond SF regions Distribution, composition Morphology of the ISM 18

DM: Community-based BB Projects Main survey Faint quasar spectroscopy across the sky Unprecedented absorber statistics Needles in the haystack May require targeting non-standard sources

20 DM: Community-based BB Projects Main survey Faint quasar spectroscopy across the sky Unprecedented absorber statistics Needles in the haystack May require targeting non-standard sources Piggy-back mode Community fibers Key for rare objects on the sky Full instrument High-spatial mapping of diffuse medium Requires high-density of sources Challenging for absorption studies 19

21 DM: Community-based BB Projects Getting the ball rolling... 20

IGM/Galaxy Connection at z<1 Tripp+11 Normalized Flux (+offset) N a (v) [10 12 cm!2 (km/s)!1 ] 6 4 2 0 3 0 4 Mg II 2796.4Å N III 685.0Å N IV 765.2Å N V 1238.8Å N V 1242.8Å Ne VIII 770.4Å Ne VIII 780.

22 IGM/Galaxy Connection at z<1 Tripp+11 Normalized Flux (+offset) N a (v) [10 12 cm!2 (km/s)!1 ] Mg II Å N III 685.0Å N IV 765.2Å N V Å N V Å Ne VIII 770.4Å Ne VIII 780.3Å 6 N V Å Å 2 0!600!400! Absorber Velocity (km s!1 ) Ne VIII 770.4Å 780.3Å Science CGM characterization Environment/gas connection Galactic feedback Mapping the cosmic web Observations HST/COS will obtain exquiste UV spectra of several 10 s quasars High S/N Coverage of range of ionization states Dedicated+deep galaxy survey on small and medium scales 100kpc to tens of Mpc sub-l* => R~23mag 21

23 Characterizing Galactic-Winds at z~0.5 Science Nature of feedback across cosmic time z~0, z~1, z>2 are under heavy study Connect to galaxy properties (AGN,SF) Observations Target 50,000+ SF galaxies at z~0.5 e.g. 10 dedicated fibers per BB pointing r<22mag with S/N~1 in the continuum Coverage of FeII, MgII, NaI absorption Stacked spectra (for most analysis) BOSS project underway Ancillary Incredible dataset for studying SF galaxies at modest redshift Galaxy/galaxy tomography Can this be extended to z>1? Rubin+10 22

CGM of galaxies Propagation of metals to the IGM

Observations Require probes (ideally multiple) on

coverage of FeII, MgII Need target galaxies (see

fibers Could re-map BB fields too LRGs too

24 Mapping the CGM at z~ kpc Science Census of metals, dust, gas in the CGM of galaxies Propagation of metals to the IGM (feedback) Reservoir for future SF ( recycling ) Observations Require probes (ideally multiple) on projected scales of a few hundred kpc BB provides coverage of FeII, MgII Need target galaxies (see previous slide) Rare configurations => Select fibers Could re-map BB fields too LRGs too Background sources Quasars, SF galaxies Leverage existing SDSS/BOSS spectra Stacked and individual spectra 23

Close QQ and QG Pairs at all z Science CGM of quasars and galaxies Gas, metal, dust distributions Small-scale feedback processes IGM thermal history, enrichment Quasar triggering Galaxy/galaxy

25 Close QQ and QG Pairs at all z Science CGM of quasars and galaxies Gas, metal, dust distributions Small-scale feedback processes IGM thermal history, enrichment Quasar triggering Galaxy/galaxy mergers Observations Target any/all sources within a few arcseconds of a known QSO SDSS and BOSS Ancillary Tremendous follow-up value Arcseconds H! [OIII]"" 4959, Observed Wavelength [Å] 0 h 1 kpc 24

Needles Science Highly enriched gas Dust production; nucleosynthesis Metal-free gas BBN; feedback; PopIII stars HeII reionization High z IGM Observations Targeting matters Quasars with highly

26 Needles Science Highly enriched gas Dust production; nucleosynthesis Metal-free gas BBN; feedback; PopIII stars HeII reionization High z IGM Observations Targeting matters Quasars with highly reddened color Quasars within the stellar locus Fainter quasars at z>4 BB offers an unprecedented opportunity to target the unknown Z ( Z O )!/! mean Jian-Guo+11 Fumagalli Number density (cm -3 ) 25

High S/N spectra for NaI, CaII absorption Not optimal ions, but only options Examine

27 Small-scale structure of the ISM Science Density structure of the neutral ISM Morphology of atomic clouds Observations Target large stellar clusters on the sky Open clusters? High S/N spectra for NaI, CaII absorption Not optimal ions, but only options Examine kinematic, spatial variations Ancillary High S/N spectra will enable characterization of stellar atmospheres 26

galaxies Large angular extent ~100kpc in the BB field-of view Target (R<22 sources)

28 Extinction Maps of Local Galaxies Science Galactic-scale feedback Traced by metals/dust Dust formation/destruction Characterization of the diffuse ISM Observations Choose nearby galaxies Large angular extent ~100kpc in the BB field-of view Target (R<22 sources) Galactic stars -- Galactic extinction Quasars, red-and-dead galaxies Photometry will be essential 27

Gas Accretion & Outflows from Redshift z~1 Galaxies

Gas Accretion & Outflows from Redshift z~1 Galaxies David C. Koo Kate Rubin, Ben Weiner, Drew Phillips, Jason Prochaska, DEEP2, TKRS, & AEGIS Teams UCO/Lick Observatory, University of California, Santa