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Home , GALEX, SPHEREx, TRACE

SPHEREx: An All-Sky Spectral Survey

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

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

Low-Risk Implementation ▪ Single Observing Mode ▪ No Moving Parts ▪ Large Technical & Scientific Margins SPHEREx Science Themes

How did the Universe begin? New constraints on non-Gaussianity

What are the conditions for life How did galaxies begin? outside the system? Deep intensity mapping fields Survey of interstellar ices SPHEREx Creates an All-Sky Legacy Archive A spectrum for every 6″ pixel on the sky

Medium- High- Accuracy Accuracy Detected Spectra Spectra Clusters > 1 billion > 100 million > 10 million 100,000 All-Sky surveys demonstrate high scientific returns with a lasting data legacy used across astronomy Galaxies

Main COBE Sequence Brown Spectra Dust-forming Dwarfs Cataclysms IRAS > 100 million 10,000 > 400 > 1,000 GALEX WMAP

Stars WISE Asteroid & Comet Galactic Quasars Quasars z >7 Spectra Line Maps More than 1.8 million total citations > 1.5 million 2 – 300? 100,000 PAH, HI, H2

Other SPHEREx science: Doré et al. 2014 SPHEREx workshops: Doré et al. 2016 & 2018 SPHEREx Overview High-Throughput LVF Spectrometer

Linear Variable Filter

Focal Plane Assembly

Spectra obtained by stepping source over the -18 -2 Speed ≡ 1/(time to map full sky to dF = 10 Wm ) FOV in multiple images: no moving parts Power ≡ ∫ Speed (dl/l) How Do We Probe Physics? Observables ● Inflationary gravitational waves – CMB “B-mode” polarization ● Spectral index of fluctuations – CMB and large-scale structure ● Non-Gaussianity – Sensitive to Inflaton field, single- or multi-field

2 f = flinear + fNL f linear CMB: fNL < 10.8 (2s)

Local fNL; Planck 2015 results Large-Scale Structure will give best non-Gaussianity measurements

Non-Gaussianity appears on largest spatial scales – need large volume survey SPHEREx Large Volume Survey

Catalog Split into Accuracy Bins SPHEREx Surveys Maximum Cosmic Volume

sz/(1+z)

SPHEREx Large-Volume Redshift Catalog • Largest effective volume of any survey, near cosmic limit • Excels at z < 1, complements dark energy missions (Euclid, WFIRST) targeting z ~ 2 • SPHEREx + measures gravitational lensing and calibrates Euclid photo-zs Survey Designed for Two Tests of Non-Gaussianity • Large scale power from power spectrum: large # of low-accuracy • Modulation of fine-scale power from bispectrum: fewer high-accuracy redshifts COMPLEMENTARITY BETWEEN NON- GAUSSIANITY AND B-MODES Single-field models from CMB-S4 Science paper Primordial non-Gaussianity discriminates between models Single-field inflation → fNL << 1 Multi-field inflation → fNL ≳ 1 Cyclic models → fNL ~ 1 (Steinhardt, Ijjas)

de Putter, Gleyzes, Doré 16

Multi-field models • Multi-field with primordial perturbations generated by inflaton • Primordial perturbations generated by second field (i.e. spectator-dominated models) SPHEREX AND INFLATION

• SPHEREx improves non- Gaussianity accuracy by a factor of ~10 Improves ΔfNL ~ 5 accuracy today to ΔfNL < 0.5

• SPHEREx optimized for non- Gaussianity measurement Broad redshift range Survey designed to cover large spatial scales Two independent tests of non-Gaussianity: - Power spectrum (PoS) - Bispectrum (BiS) CMB LENSING CROSS-CORRELATION • The SPHEREx galaxy clustering

measurement covers the full sky and G )/D G

is cosmic variance limited on large (D s ~ g

scales b )/ g b ( s

• SPHEREx determines galaxy bias bg from the galaxy power spectrum analysis

• Given bg, Galaxy x CMB lensing: Measures the growth of structure DG over a wide redshift range -- Probes gravity on large scales -- Constrains the amplitude Alens

Calculation by E. Schaan Doré, Werner++16 KSZ CROSS-CORRELATION

• SPHEREx + CMB-S4 greatly increase our ability to measure the baryon component of the kinematic Sunyaev-Zel’dovich effect

• Using the velocity reconstruction method, and using only the two highest redshift accuracy (~24.5M galaxies) S/N~55 assuming half the sky (CMB map noise of 14 μK-arcmin)

• Using direct cross-correlation between T2 and δgal (Doré++03, Hill++16, Ferraro++16) allows a statistical measurement with less stringent requirements on redshift errors: S/N > 100 can be achieved by combining SPHEREx with future CMB experiments

Calculation by S. Ferraro & E. Schaan Doré, Werner++16 CLUSTER IDENTIFICATION AND REDSHIFTS

mission will discover 100,000 massive systems • CMB-S4 + eROSITA will find 100,000+ massive clusters contain no redshift information auxiliary data are required

• SPHEREx cluster redshift errors* over the full sky will Equal or exceed current optical surveys for redshifts z < 0.6 Give σ(z)/(1 + z) < 0.03 for z < 0.9 Provide virial masses for large SPHEREx errors statistical cluster sample

• SPHEREx will also find ~30,000 clusters independently

Doré, Werner++16 *Cluster redshift errors simulated by Lindsey Bleem SPHEREx Science Team Jamie Bock Caltech/JPL Principal Investigator Rachel Akeson IPAC Stellar catalog Matt Ashby CfA Interstellar ices Lindsey Bleem Argonne Galaxy cluster catalog IPAC Galaxy redshifts Tzu-Ching Chang JPL Intensity mapping Asantha Cooray UC Irvine Extragalactic backgrounds Brendan Crill JPL Pipeline architect Roland de Putter Caltech Cosmology Olivier Doré JPL Project Scientist Tim Eifler JPL/U. Arizona LSST/DESI synergies Thanks Salman Habib Argonne Cosmology simulations Katrin Heitmann Argonne Cosmology simulations Chris Hirata Ohio State Cosmology Woong-Seob Jeong KASI KASI PI for Davy Kirkpatrick IPAC Brown dwarfs Phil Korngut Caltech Instrument Scientist Elisabeth Krause JPL/U. Arizona Cosmology Carey Lisse JHU Solar system catalog Listening! Daniel Masters Caltech Spectral redshift fitting Phil Mauskopf Arizona State Survey planning Gary Melnick CfA Interstellar ices Hien Nguyen JPL Instrumentation Karin Öberg CfA Ice properties Roger Smith Caltech Detector arrays Yong-Seon Song KASI Cosmology Harry Teplitz IPAC/Caltech Data Archive Volker Tolls CfA Ices pipeline Steve Unwin JPL Interstellar ices Mike Werner JPL Legacy science Rogier Windhorst Arizona State JWST synergies Yujin Yang KASI Survey science Mike Zemcov RIT Data pipeline Measuring Primordial Non-Gaussianity to σ(fNL) < 1 A test to distinguish between single- and multi-field Inflation Single-Field Inflation:

ΦS

ΦS Squeezed limit consistency condition by Φ Maldacena (2003): (infl) L fNL ~ (ns −1) <<1 Non-Gaussianity Produces Two Signatures Multi-Field Inflation: Enhanced power on large spatial scales FL

Modulated small-scale power FS on large scales FL due to non-linear mode coupling

- measured with power spectrum and bispectrum

(infl) fNL ≥1 Redshifts with SPHEREx We extract the spectra of known sources using the full-sky catalogs from PanSTARRS/DES. Controls blending and confusion We compare this spectra to a template library (robust for low redshift sources): WISE For each galaxy: redshift & type Multiple types test galaxy bias effects PanSTARRS The 1.6 μm bump is a well known universal photometric indicator (Simpson & Eisenhardt 99) We simulated this process using the COSMOS data set using the same process as Euclid/WFIRST (Stickley et al.). The power of low-resolution spectroscopy has been demonstrated with PRIMUS (Cool++14), COSMOS (Ilbert++09), NMBS (van Dokkum++09). Testing Redshift Reliability Inject Real Galaxies into SPHEREx Pipeline Input Deep Galaxy Catalog Preparation Example Template and Redshift Fits 30 band observations of the Each galaxy and is SPHEREx simulation input Published COSMOS catalog: COSMOS-based deep COSMOS field from HST, photometric catalog with assigned a best fit SED Subaru, Spitzer, GALEX, template using measured galaxy catalog (position, SED, measured spectroscopic or redshift, luminosity, flux in all Subaru, CFHT, Chandra, photometric redshift and redshift and data-based SED Keck template library SPHEREx, Pan-STARRS, DES and stellar types WISE bands) Image Simulation Generate 8x spatially-oversampled Convolve with three different images at SPHEREx’s 96 spectral Gaussians to account for Add instrumental noise plus overall and source-by-source calibration Simulated channels summing the emission of diffraction, wave-front Images all galaxies in every pixel error at 0.75 µm, and pointing jitter errors (Table M.5.3-4) over 150 seconds Source Extraction Use sources detected in Measure fluxes in each Simulated Pan-STARRs or DES to define Exclude sources where Remove confusion SPHEREx band using Galaxy SPHEREx galaxy sample and blending is important mean offset estimate forward modeling with Catalog the associated astrometry Tractor Fluxes Spectroscopic Redshift Estimation Use SED template library from Brown et al. (or Galaxy catalog with associated SED template, SPHEREx others) to fit each galaxy’s SPHEREx and dust extinction, luminosity, redshift, associated Spectroscopic Pan-STARRS fluxes errors and goodness of fit Catalog Parameter Forecasts Assign each bin a Compute errors on Marginalize over SPHEREx Inflation Discard galaxies PoS and BiS in galaxy bias using Compute errors for Investigation with poor published each wavelength bias and other redshift accuracy parameters Cosmological goodness of fit bins CFHT/COSMOS and redshift bins Forecasts data prescriptions Resulting Redshift Errors Mapping the Sky with LVFs 1 orbit

Spectral

2 orbits

N orbits

A complete spectrum is made from a series of images SPHEREx maps the sky over multiple orbits with large and small slews SPHEREx All-Sky Survey Data Products & Tools Planned Data Releases Survey Data Date (Launch +) Associated Products Rapid Data + 2 mo Spectral images Survey 1 1 – 8 mo S1 spectral images Survey 2 8 – 14 mo S1/2 spectral images Early release catalog Survey 3 14 – 20 mo S1/2/3 spectral images Survey 4 20 – 26 mo S1/2/3/4 spectral images Final Release Legacy catalogs and maps Available Data Tools Analysis Tool Function Image lookup Find image at location and time Forced photometry Spectrum at a known source position Data cube viewer View images of any sky region On-the-fly mosaic Images at specified time & place Variable sources Spectra at provided positions & times Source discovery Catalog of blind source detections Legacy Catalogs and Maps Catalog # Function Notable Features of the SPHEREx All-Sky Survey Core science > 490 M Galaxy types & redshift • High S/N spectrum for every 2MASS source catalogs > 700,000 Ice sources Deep field maps Image mosaics • Solid detection of faintest WISE sources Stars > 100 M SEDs of known stars • Catalogs ideal for JWST observations Galaxies 1.4 B SEDs of known galaxies Clusters 100,000 SEDs of cluster members Asteroids 100,000 SEDs of known objects Galaxy maps Image and line mosaics *more releases, tools and catalogs under consideration SPHEREx Measures Large-Scale Fluctuations Fluctuations in Continuum Bands Fluctuations in Lines

• Emission lines encode clustering signal • SPHEREx has ideal wavelength coverage at each redshift over cosmic history and high sensitivity • Amplitude gives line light production • Multiple bands enable correlation tests • Multiple lines history sensitive to redshift history - High S/N in Ha for z < 5; OIII and Hb for z < 3 • Method demonstrated on Spitzer & CIBER - Lya probes EoR models for z > 6 - Ha and Lya crossover region 5 < z < 6 SPHEREx Surveys Ices in All Phases of Star Formation

Young Stellar Envelopes

Dense Clouds

Young Solar Systems Protoplanetary Disks What Would You Do with the Archive?

Science Synergies 2018 Workshop at CfA - JWST, eROSITA, Euclid, , PLATO, TESS, WFIRST - ALMA, HERA, LSST, SKA

New Ideas from the 2016 Workshop Object # Sources Legacy Science Reference 2016 Workshop: Over 50 non-SPHEREx scientists X-ray all-sky > 100,000 Detect eROSITA source SEDs Dore et al. 2016 and spectroscopic redshifts survey Charter: Identify new science, tools and data products Missing baryons > 10,000 In conjunction with CMB, Dore et al. 2016 detect kSZ signal in galaxy Ferraro et al. 2016 2014 SPHEREx science paper: Over 60 citations groups and clusters Exoplanet 10,000 With GAIA, determine Dore et al. 2016 Workshop white paper: 84 pages, 68 authors precise radii for host stars characterization Deuterated Probe and possible map Dore et al. 2016 deuterated PAHs, complete Doney et al. 2015 PAHs inventory of D in local ISM Lowest ~1000 Identify low-mass stars by Dore et al. 2016 their IR signatures, map metallicity stars distribution in Galaxy Asteroids and 100,000 Spectrally classify numerous Dore et al. 2016 asteroids; CO/CO2 ratios in comets comets Nearby galaxies >100 million Spectrally image galaxies to 2MASS catalogs trace stellar populations, star formation, etc New idea here! TBD Exoplanet masses X-ray synergies .caltech.edu

SPHEREx Tests Inflationary Non-Gaussianity

1s errors SPHEREx (MEV) Planck statistical Euclid & (systematics) PoS BiS PoS+BiS PoS BOSS

SPHEREx fNL Req’t 1.15 0.55 0.5 N/A N/A 0.89 0.35 0.32 fNL (0.53) (0.22) (0.21) 5.6 5.0 Spectral Index ns 2.7 1.9 1.1 2.6 4.0 (´10-3) - Running as (´10 3) 1.0 0.9 0.25 1.1 13

Curvature Wk 7.7 8.1 4.4 7.0 40 (´10-4) Dark Energy figure of merit (bigger is better) 371 309 14

• Projected SPHEREx sensitivity is DfNL < 0.5 (1s) - Two independent tests via power spectrum and bispectrum • Competitively tests running of the spectral index • SPHEREx low-redshift catalog is complementary for dark energy