An All-‐Sky Spectral Survey

SPHEREx: An All-Sky Spectral Survey

Designed to Explore ▪ The Origin of the Universe ▪ The Origin and History of Galaxies ▪ The Origin of Water in Planetary Systems

The First All-Sky Near-IR Spectral Survey A Rich Legacy Archive for the Astronomy Community with 100s of Millions of Stars and Galaxies

Low-Risk Implementaon ▪ No Moving Parts ▪ Single Observing Mode ▪ Large Technical & Scienfic Margins ▪ Follows successful CIT/JPL mgt. model of NuSTAR What are the Most Important Quesons in Astrophysics? As Stated in the NASA 2014 Science Plan

How Did the Universe Begin? “Probe the origin and destiny of our universe, including the nature of black holes, dark energy, dark matter and gravity”

How Did Galaxies Begin? “Explore the origin and evolution of the galaxies, stars and planets that make up our universe”

What are the Condions for Life Outside the Solar System? “Discover and study planets around other stars, and explore whether they could harbor life” SPHEREx Creates an All-Sky Legacy Archive Legacy Science Opportunies: A Few Examples Object # Sources Legacy Science Reference Detected 1.4 billion Properes of distant and heavily obscured galaxies galaxies Galaxies 120 million Study (H, CO, O, S, H2O) line and PAH emission by Simulaon σ(z)/(1+z) galaxy type. Explore galaxy based on < 0.03 and AGN life cycle COSMOS and Pan-STARRS Galaxies σ 9.8 million Cross check of Euclid photo-z. Measure (z)/(1+z) dynamics of groups and < 0.003 map filaments. QSOs > 1.5 million Understand QSO lifecycle, environment, and taxonomy Ross et al. QSOs 0-300 Determine if early QSOs (2013) plus exist. Follow-up spectro- simulaons at z > 7 scopy probes EOR through Lyα forest Clusters with 25,000 Redshis for all X-ray Geach et al., clusters. Viral masses and 2011, SDSS ≥ 5 members merger dynamics counts Main >100 million Test uniformity of stellar 2MASS mass funcon within our catalogs sequence Galaxy as input to stars extragalacc studies Mass-losing, Over 10,000 Spectra of M supergiants, Astro-physical OH/IR stars, Carbon stars. Quanes, 4th Notable Features of the SPHEREx All-Sky Survey dust forming of all types Stellar atmospheres, dust edion [ed. stars return rates, and A.Cox] p. 527 • High S/N spectrum for every 2MASS source composion of dust Brown >400, incl. Atmospheric structure and dwarfarchives. • Solid detecon of faintest WISE sources composion; search for org and J.D. dwarfs >40 of types hazes. Informs studies of Kirkpatrick, • Catalogs ideal for JWST observaons T and Y giant exoplanets priv. comm. Stars with >1000 Discover rare dust clouds Kennedy & produced by cataclysmic Wya (2013) hot dust events like the collision which produced the Earth’s moon New ideas recently brought to our aenon Diffuse ISM Map of the Study diffuse emission GLIMPSE from interstellar clouds survey • Redshis for the all-sky eRosita X-Ray survey Galaxy and nebulae; (H, CO, S, (Churchwell H O and PAH emission) • Photo baselines for wide-field transient survey 2 et al. 2009) • Mapping 3D distribuon of Galacc ices And there’s more! SPHEREx: Simple Instrument, Large Margins Deployed Wide-field thermal telescope shields 20 cm eff. aperture

High-throughput spectrometer Passive uses a linear-variable filter in cooling front of each detector array 185 cm system

BCP 100 spacecraft Deployed Solar Instrument Specificaons panels Parameter Value Telescope Effecve Aperture 20 cm Pixel Size 6.2" x 6.2" Field of View 2 x (3.5° x 7.0°); dichroic Large Resource Margins Spectrometer Linear-Variable Filters Observatory Mass 53 % Resolving Power and R=41.5 λ=0.75 - 4.1 µm Observatory Power 36 % Wavelength Coverage R=150 λ=4.1 - 4.8 µm Poinng Stability 43 % 2 x Hawaii-2RG 2.5 µm Arrays 2 x Hawaii-2RG 5.3 µm Cooling Power 450 % Point Source Sensivity 18.5 AB mag (5σ) with Science Overall 300 % (MEV Performance) 300% margin to req’t Cooling All-Passive Why Study Ices? Schematic of a protoplanetary disk r apo e • Gas and dust in molecular er V n Wat i ne r of L o clouds are the reservoirs for new Laye ow Z ace Sn ce stars and planets Surf I - In molecular clouds, water is Formation of icy Planetesimals 100-1000x more abundant in ice Star than in gas Diffusive Transport - Herschel observations of the TW of Water? 0au 0.1au 1.0au Hydrae disk imply the presence of 10au 1000s of Earth oceans in ice (Hogerheijde et al. 2011) ISO absorption spectrum - Models suggest water and biogenic molecules reside in ice in the disk mid-plane and beyond

the snow line

• Ideal λs to study ices: 2.5 - 5 µm - Includes spectral features from

H2O, CO and CO2 - Plus chemically important minor

constituents NH3, CH3OH, X-CN, 13 and CO2 SPHEREx Galacc Ice Survey SPHEREx will be a game changer to Ices in each Phase of Star Formation

g resolve long-standing questions about O C N C SPHEREx X the amount and evolution of key O 2 Galactic C H O Ice H 3 biogenic molecules through all phases C O Survey H 2 ! H 3 of star and planet formation N • SPHEREx increases the number of ice spectra from ~200 to >> 20,000 • Band 4 spectral resolving power λ/ Δλ = 150 chosen to isolate the absorption from each ice species

The SPHEREx ice catalog will: One Million Targets with |b| < 1° • Contain molecular clouds, YSOs, and 1000s of protoplanetary disks • Determine the role of environment (T, n, radiation field, cosmic rays) in forming ices • Determine if ices in disks come from the parent cloud or are reformed • Measure the abundance of water and biogenic ices in disks that is available to new planets Why Study the Extragalacc Background Light?

Origin of CMB Dark Ages Epoch of Reionization: First Stars Form Modern Galaxies Today Big Bang

EBL from ReionizationReionizaon EBL EBL from galaxies EBL from galaxies 400 kyr 500 Myr 1 Gyr 5 Gyr 13 Gyr Time

Epoch of Reionizaon Observables When did it begin? Free Electrons: Scaer CMB photons When did it end? Neutral Gas: HI 21 cm, Ly absorpon What were the first sources like? Galaxies: Stellar light, line emission Measure Extragalacc Background Via Spaal Variaons

Herschel (FIR wavelengths) Spitzer Amblard et al. 2011 Kashlinsky et al. 2005 Viero et al. 2013 Cooray et al. 2012

arcmin CIBER 12 x 6 Zemcov et al. 2014 Akari Matsumoto et al. 2010 10 arcmin

2°

m m 1.0 µ 1.6 µ

Successful Applicaons at Longer Wavelengths Herschel EBL: Viero et al. 2013 Planck EBL: Planck C. et al. 2013 Planck EBL x CMB Lensing: Planck C. et al. 2014 Herschel EBL x CMB Lensing: Many 2.4 um 3.2 um Measuring Cosmic Light Producon What Constutes Cosmic Light Producon? Fluctuaons in Connuum Bands

Moseley & Zemcov 13+ billion years of galaxy Diffuse emission between Science 2014 collisions and mergers galaxies from tidally stripped stars

Inflation fraction of a trillionth of a second

Cosmic microwave background ~380,000 years First stars & galaxies ~400 million years Present universe ~13.8 billion years 1) Photon Producon in Galaxies Nucleosynthesis & black holes, peaks at z ~ 2 • SPHEREx has ideal wavelength coverage 2) First Stars and Galaxies and high sensivity Epoch of Reionizaon z > 6 • 3) Inter Halo Light Mulple bands enable correlaon tests Tidally stripped stars at z = 0 - 2 sensive to redshi history 4) Surprises? • Method demonstrated on CIBER, Spitzer, E.g. Light from parcle decay AKARI, Herschel, Planck Tests of Inflaon from the CMB: • Universe is geometrically flat • There are coherent structures larger than the classical horizon • Fluctuaons have a nearly “scale invariant” spectrum but with a slight departure as predicted • Density and velocity fluctuaons are in phase • Fluctuaons have Gaussian stascs How to Probe the Physics that Caused Inflaon? Observables: Inflaonary gravitaonal waves – CMB “B-mode” polarizaon Spectral index of fluctuaons – CMB and large-scale structure Non-Gaussianity – Sensive to Inflaton field (single-field vs. mul-field)

Large-scale structure will give the best non-Gaussianity measurements Effect is on largest scales: Need large volume survey Measuring Primordial Non-Gaussianity to σ(fNL) < 1 A test to disnguish between single- and mul-field Inflaon Single-Field Inflaon:

ΦS

ΦS Squeezed limit consistency condion by Φ Maldacena (2003): (infl) L fNL ~ (ns !1) <<1 Non-Gaussianity Produces Two Signatures Mul-Field Inflaon:

Modulated small-scale power ΦS on large scales ΦL due to non-linear mode coupling - measured with galaxy bispectrum

Enhanced galaxy clustering on large spaal scales - measured with galaxy power spectrum and bispecrum (infl) fNL !1 SPHEREx Large Volume Galaxy Survey SPHEREx Surveys Maximum Cosmic Volume Catalog Split into Redshi Accuracy Bins

σz/(1+z)

SPHEREx Large-Volume Redshi Catalog • Largest effecve volume of any survey, near cosmic limit • Excels at z < 1, complements dark energy missions (Euclid, WFIRST) targeng z ~ 2 • SPHEREx + Euclid measures gravitaonal lensing and helps calibrate Euclid photo-zs Survey Designed for Two Tests of Non-Gaussianity • Large scale power from power spectrum: large # of low-accuracy redshis • Modulaon of fine-scale power from bispectrum: fewer high-accuracy redshis SPHEREx Tests Inflaonary Non-Gaussianity

• Non-Gaussianity disnguishes between mul- and single-field models

• Projected SPHEREx sensivity is δfNL < 1 (2σ) - Two independent tests via power spectrum and bispectrum • Compevely tests running of the spectral index • SPHEREx low-redshi catalog is complementary for dark energy Thanks for Listening! SPHEREx:

Designed to Explore ▪ The Origin of the Universe ▪ The Origin and History of Galaxies ▪ The Origin of Water in Planetary Systems

The First All-Sky Near-IR Spectral Survey A Rich Legacy Archive for the Astronomy Community with 100s of Millions of Stars and Galaxies

Low-Risk Implementaon ▪ No Moving Parts ▪ Single Observing Mode ▪ Large Technical & Scienfic Margins ▪ Follows successful CIT/JPL mgt. model of NuSTAR