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Olivier Doré JPL/Caltech SPHEREx Olivier Doré JPL/Caltech for the SPHEREx team http://spherex.caltech.edu Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 1 SPHEREX HAS THREE CORE SCIENCE THEMES NASA Goal: Probe the origin and destiny of the Universe SPHEREx maps the large scale structure of galaxies to study the inflationary birth of the universe Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 2 SPHEREX HAS THREE CORE SCIENCE THEMES NASA Goal: Probe the origin and destiny of the Universe SPHEREx maps the large scale structure of galaxies to study the inflationary birth of the universe NASA Goal: Explore whether planets around other stars could harbor life SPHEREx determines the abundance of interstellar water and organic ices available to proto-planetary systems Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 2 SPHEREX HAS THREE CORE SCIENCE THEMES NASA Goal: Probe the origin and destiny of the Universe SPHEREx maps the large scale structure of galaxies to study the inflationary birth of the universe NASA Goal: Explore whether planets around other stars could harbor life SPHEREx determines the abundance of interstellar water and organic ices available to proto-planetary systems NASA Objective: Explore the origin and evolution of galaxies SPHEREx measures the total light produced by stars and galaxies over cosmic history Also talk by Tzu-Ching Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 2 SPHEREx: An All-Sky Spectral Survey Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer A high throughput, low-resolution near-infrared spectrometer. Credit IPAC/2MASS Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 3 SPHEREx: An All-Sky Spectral Survey Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer A high throughput, low-resolution near-infrared spectrometer. λ Credit IPAC/2MASS Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 3 SPHEREX: AN ALL-SKY SPECTRAL SURVEY Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer A high throughput, low-resolution near-infrared spectrometer. SPHEREx Dataset: For every 6.2” pixel over the entire sky: ➡ R=40 spectra spanning (0.75 μm < λ < 4.18 μm). ➡ R=150 spectra (4.18 μm < λ < 5.0 μm). O.D., Bock et al., arXiv:1412.4872 Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 4 SPHEREX SURVEY DEPTH Deep survey Current Best Estimated Full-sky survey Maximum Estimated Value Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 5 SPHEREX PROVIDES A RICH ALL-SKY SPECTRAL ARCHIVE Detected Med. High Accuracy Clusters > 1 Accuracy z’s z’s 25,000 billion > 100 million 10 million All-Sky surveys demonstrate high scientific returns with a Galaxies Main Seq. Dust-forming Brown lasting data legacy used Spectra Cataclysms 10,000 Dwarfs > 1,000 across astronomy > 100 million > 400 COBE Stars IRAS Quasars Quasars z >7 Asteroid Galactic Line GALEX > 1 million 2 – 300? Spectra Maps WMAP 10,000 PAH, HI, H 2 Planck WISE Other Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 6 SPHEREx DESIGN An Innovative Architecture Based on Mature Technologies Compact spectrometer Wide field telescope Passive cooling system 185cm Parameter Value Telescope eff. diameter 20 cm Field of view 3.5 x 711.3 degree degree Pixel size 6.2 arcsec Wavelength range 0.75 – 5 µm Ball BCP 100 Spacecraft Bus Resolving power l/Dl 41 - 135 Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 7 High-ThroughputHigh%Throughput,LVF,Spectrometer, LVF Spectrometer Linear&Variable&Filter& 2.5 µm H2RG Arrays in t t1 t3 t Band t1 Band t3 Band Focal&Plane&Assembly& λ = 0.75 – 1.11 λ = 1.11 – 1.64 λ = 1.64 – 2.42 t1 t3 t4 5 µm H2RG Arrays in t t1 t3 t Band t1 Band t3 Band Methane&on&Pluto& 1.0& 3.5 0.8& 0.6& λ = 2.42 – 3.68 λ = 3.68 – 4.45 λ = 4.45 – 5.01 I/F& 0.4& t1 t3 t4 0.2& 0.0& 11.3 1.6&&&&&&&&&&&&&1.8&&&&&&&&&&&&&2.0&&&&&&&&&&&&&2.2&&&&&&&&&&&&2.4& Infrared&Spectral&Image& Wavelength&(µm)& LVFs&used&on&ISOCAM,&HSTPWFPC2,& Spectra&obtained&by&stepping&source&over&the& New&Horizons&LEISA,&&&OSIRIXPReX&(2016&launch)& FOV&in&mul;ple&images:&&no,moving,parts, Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 8 High-ThroughputHigh%Throughput,LVF,Spectrometer, LVF Spectrometer Linear&Variable&Filter& 2.5 µm H2RG Arrays in t t1 t3 t Band t1 Band t3 Band Focal&Plane&Assembly& λ = 0.75 – 1.11 λ = 1.11 – 1.64 λ = 1.64 – 2.42 t1 t3 t4 5 µm H2RG Arrays in t t1 t3 t Band t1 Band t3 Band Methane&on&Pluto& 1.0& 3.5 0.8& 0.6& λ = 2.42 – 3.68 λ = 3.68 – 4.45 λ = 4.45 – 5.01 I/F& 0.4& t1 t3 t4 0.2& 0.0& 11.3 1.6&&&&&&&&&&&&&1.8&&&&&&&&&&&&&2.0&&&&&&&&&&&&&2.2&&&&&&&&&&&&2.4& Infrared&Spectral&Image& Wavelength&(µm)& LVFs&used&on&ISOCAM,&HSTPWFPC2,& Spectra&obtained&by&stepping&source&over&the& New&Horizons&LEISA,&&&OSIRIXPReX&(2016&launch)& FOV&in&mul;ple&images:&&no,moving,parts, Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 8 Mapping the Sky with LVFs 1 orbit Spectral image 2 orbits N orbits SPHEREx maps the sky over multiple A complete spectrum is made from a series of images orbits with large and small slews Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 9 ASTRONOMY IN THE INTENSITY MAPPING REGIME Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 10 ProbingInstead:))Probe)EBL)by)Studying) the EBL with Spatial FluctuationsSpa$al&Varia$ons& in NIR or mm •Herschel)(FIR)wavelengths))W Spitzer) Amblard*et*al.*2011* Kashlinsky*et*al.*2005* Viero*et*al.*2013* Cooray*et*al.*2012* * Planck CIB map arcmin 12*x*6* Akari) Planck)(Lensing)map)) Matsumoto*et*al.*2010* 10*arcmin* Planck*C.*et*al.*2014* Successful)Applica=ons)at)Longer)Wavelengths) *****Herschel*EBL:**Viero*et*al.*2013* *****Planck*EBL:**Planck*C.*et*al.*2013* XXX *****Planck*EBL*x*CMB*Lensing:**Planck*C.*et*al.*2014* XVIII *****Herschel*EBL*x*CMB*Lensing:**Many ** 2.4*um* 3.2*um* Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 11 PROBING THE EPOCH OF REIONIZATION Fluctuations in Continuum Bands • SPHEREx orbits enable deep/frequent observations of about 200 sq. deg near the ecliptic poles (great for systematics!) Current Measurements • SPHEREx wavelength coverage and 1 σ resolution will enable large-scale measurement of spatial fluctuations in the Extragalactic Background Light (EBL). • In particular, SPHEREx will monitor/explain the Intra-Halo Light and its evolution (CIBER, Zemcov++14). • SPHEREx has the raw sensitivity to probe the expected EOR signal (but separation with low z signal will be challenging). • The sensitivity in this region will enable deep intensity mapping regimes using multiple lines at all redshift, and maybe Lyα at high redshift (see Croft++15) see Tzu-Ching’s talk tonight Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 12 SPHEREX TEAM Jamie Bock (PI) Caltech/JPL Roland de Putter JPL Matt Ashby CfA Tim Eifler JPL Peter Capak IPAC Rachel Akeson IPAC Asantha Cooray UC Irvine Yan Gong UC Irvine Brendan Crill JPL/Caltech Lindsey Bleem Argon Olivier Doré (PS) JPL/Caltech Daniel Masters Caltech Chris Hirata OSU Phil Mauskopf ASU Woong-Seob Jeong KASI Tzu-Ching Chang JPL/Caltech Minjim Kim KASI Hien Nguyen JPL Phil Korngut (IS) Caltech Karin Öberg CfA Elisabeth Krause Stanford Davy Kirkpatrick IPAC Dae-Hee Lee KASI Harry Teplitz IPAC Gary Melnick CfA Volker Tolls CfA Roger Smith Caltech Salman Habib Argonne Yong-Seon Song KASI Katrin Heitmann Argonne Stephen Unwin JPL Karin Sandstrom UCSD Michael Werner JPL Carey Lisse JHU Michael Zemcov Caltech Rogier Windhorst ASU Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 13 SPHEREX WILL ENABLE ROBUST AND UNIQUE SCIENCE INVESTIGATIONS •SPHEREx will create the first all sky near-infrared spectroscopic survey: ➡SPHEREx will create a dataset of lasting legacy. ➡High quality archival products are now fully part of the MIDEX mission. •SPHEREx offers a simple and very robust design and modus operandi: ➡It naturally enables a high control of systematics thanks to multiple built-in redundancy. •SPHEREx will also enable other original and powerful studies on EOR: ➡The extra-galactic background light from z=0 till the reionization era. ➡Relies on broadband fluctuation measurements or line intensity mapping. •Community support is important! ➡If you want SPHEREx to happen, please mention it in your papers or talks. http://spherex.caltech.edu Olivier Doré SPHEREx Second Community Workshop - CfA, January 2018 14 FREQUENTLY ASKED QUESTIONS • The pixel size under samples the PSF, isn’t that bad? ➡ For sources for known positions, we know the PSF and pointing in each image and can do optimal forced photometry (a la Tractor). For unknown source positions yes there is some degradation of sensitivity for aperture photometry. Sensitivities quoted for sources with known positions. • How can SPHEREx be more sensitive than WISE? ➡ We checked. SPHEREx has long integrations that are photon noise limited, and fewer effective pixels in the PSF. These more than compensate for 2x smaller mirror diameter. • Isn’t SPHEREx confusion limited with 6” pixels? ➡ Confusion is minor in high-latitude sky at our sensitivity, and blended galaxies are flagged based on PS-DES and WISE images and removed from the cosmology survey.
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