Galaxy evolution probe

The Galaxy Evolution Probe (GEP) is a concept for a mid- and far-infrared space observatory to measure key properties of large samples of galaxies with large and unbiased surveys. GEP will attempt to achieve zodiacal light and Galactic dust emission photon background-limited observations by utilizing a 6-K, 2.0-m primary mirror and sensitive arrays of kinetic inductance detectors (KIDs). It will have two instrument modules: a 10 to 400  μm hyperspectral imager with spectral resolution R  =  λ  /  Δλ  ≥  8 (GEP-I) and a 24 to 193  μm, R  =  200 grating spectrometer (GEP-S). GEP-I surveys will identify star-forming galaxies via their thermal dust emission and simultaneously measure redshifts using polycyclic aromatic hydrocarbon emission lines. Galaxy luminosities derived from star formation and nuclear supermassive black hole accretion will be measured for each source, enabling the cosmic star formation history to be measured to much greater precision than previously possible. Using optically thin far-infrared fine-structure lines, surveys with GEP-S will measure the growth of metallicity in the hearts of galaxies over cosmic time and extraplanar gas will be mapped in spiral galaxies in the local universe to investigate feedback processes. The science case and mission architecture designed to meet the science requirements is described, and the KID and readout electronics state of the art and needed developments are described. This paper supersedes the GEP concept study report cited in it by providing new content, including: a summary of recent mid-infrared KID development, a discussion of microlens array fabrication for mid-infrared KIDs, and additional context for galaxy surveys. The reader interested in more technical details may want to consult the concept study report

CDIM: Cosmic Dawn Intensity Mapper Final Report

The Cosmic Dawn Intensity Mapper (CDIM) will transform our understanding of the era of reionization when the Universe formed the first stars and galaxies, and UV photons ionized the neutral medium. CDIM goes beyond the capabilities of upcoming facilities by carrying out wide area spectro-imaging surveys, providing redshifts of galaxies and quasars during reionization as well as spectral lines that carry crucial information on their physical properties. CDIM will make use of unprecedented sensitivity to surface brightness to measure the intensity fluctuations of reionization on large-scales to provide a valuable and complementary dataset to 21-cm experiments. The baseline mission concept is an 83-cm infrared telescope equipped with a focal plane of 24 x 2048^2 detectors capable of R = 300 spectro-imaging observations over the wavelength range of 0.75 to 7.5 µm using Linear Variable Filters (LVFs). CDIM provides a large field of view of 7.8 deg^2 allowing efficient wide area surveys, and instead of moving instrumental components, spectroscopic mapping is obtained through a shift-and-stare strategy through spacecraft operations. CDIM design and capabilities focus on the needs of detecting faint galaxies and quasars during reionization and intensity fluctuation measurements of key spectral lines, including Lyman-α and Hα radiation from the first stars and galaxies. The design is low risk, carries significant science and engineering margins, and makes use of technologies with high technical readiness level for space observations

A Realistic Roadmap to Formation Flying Space Interferometry

The ultimate astronomical observatory would be a formation flying space interferometer, combining sensitivity and stability with high angular resolution. The smallSat revolution offers a new and maturing prototyping platform for space interferometry and we put forward a realistic plan for achieving first stellar fringes in space by 2030

Origins Space Telescope: baseline mission concept

The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the Universe today? How do habitable planets form? How common are life-bearing worlds? To answer these alluring questions, Origins will operate at mid- and far-infrared (IR) wavelengths and offer powerful spectroscopic instruments and sensitivity three orders of magnitude better than that of the Herschel Space Observatory, the largest telescope flown in space to date. We describe the baseline concept for Origins recommended to the 2020 US Decadal Survey in Astronomy and Astrophysics. The baseline design includes a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. A mid-infrared instrument (Mid-Infrared Spectrometer and Camera Transit spectrometer) will measure the spectra of transiting exoplanets in the 2.8 to 20  μm wavelength range and offer unprecedented spectrophotometric precision, enabling definitive exoplanet biosignature detections. The far-IR imager polarimeter will be able to survey thousands of square degrees with broadband imaging at 50 and 250  μm. The Origins Survey Spectrometer will cover wavelengths from 25 to 588  μm, making wide-area and deep spectroscopic surveys with spectral resolving power R  ∼  300, and pointed observations at R  ∼  40,000 and 300,000 with selectable instrument modes. Origins was designed to minimize complexity. The architecture is similar to that of the Spitzer Space Telescope and requires very few deployments after launch, while the cryothermal system design leverages James Webb Space Telescope technology and experience. A combination of current-state-of-the-art cryocoolers and next-generation detector technology will enable Origins’ natural background-limited sensitivity

Pre-Launch Radiometric Calibration of the Ozone Mapping and Profiler Suite (OMPS) Instruments

INTRODUCTION: The Ozone Mapping and Profiler Suite (OMPS) instrument provides long-term stratospheric ozone monitoring capability for the Joint Polar Satellite System (JPSS). The JPSS OMPS instrument consists of two nadir-viewing, hyperspectral spectrometers that provide total column ozone and ozone vertical profile measurements. The first flight model of OMPS is currently on-orbit aboard the Suomi National Polar-orbiting Partnership satellite (S-NPP). The ground radiometric calibration of the OMPS instruments is discussed, which includes an overview of techniques for transferring the calibration of NIST primary standards to OMPS, in addition to a summary of the calibration uncertainties that were accounted for. OMPS SENSOR OVERVIEW: OMPS is one of five instruments that launched aboard the S-NPP satellite in 2011. A second OMPS flight unit is being built by Ball Aerospace and will fly on the Joint Polar Satellite System-1 (JPSS-1), which will launch in 2016. OMPS is a three-part instrument suite: a nadir mapper that maps global ozone with roughly 50-km ground resolution, a nadir profiler that measures the vertical distribution of ozone in the stratosphere, and a limb profiler that measures ozone in the upper troposphere and lower stratosphere with high vertical resolution [1,2]. OMPS supports operational weather capabilities by measuring the global distribution of total atmospheric ozone, and ozone concentration variability with altitude. CALIBRATION TECHNIQUES: Radiometric calibration of the OMPS spectrometer is performed on the ground by transferring the calibration of NIST primary standards to each of the sensors. OMPS is calibrated in both radiance and irradiance modes so that albedo measurements can be resolved on-orbit. On-orbit, calibration is maintained using solar measurements [3]. Each instrument has two diffusers: a working diffuser that is deployed routinely for the purpose of solar calibration, and a reference diffuser that is deployed sparingly for the purpose of monitoring working diffuser performance degradation. S-NPP PERFORMANCE: S-NPP OMPS began acquiring data on January 2012 and has continued to perform well. OMPS total column measurements have been compared to Aura OMI and EOS MLS results [4,5]. The OMPS ozone map measurements after one month of operation were consistent with OMI, and OMPS data were in agreement with EOS MLS calculated reflectances to within 1% for wavelengths \u3e 312 nm [5]. REFERENCES: [1] Dittman, Michael G., et al. Nadir ultraviolet imaging spectrometer for the NPOESS Ozone Mapping and Profiler Suite (OMPS). Proceedings of SPIE. Vol. 4814. 2002. [2] Dittman, Michael G., et al. Limb broad-band imaging spectrometer for the NPOESS Ozone Mapping and Profiler Suite (OMPS). Proceedings of SPIE. Vol. 4814. 2002. [3] Remund, Quinn P., et al. The ozone mapping and profiler suite (OMPS): on-orbit calibration design. Fourth International Asia-Pacific Environmental Remote Sensing Symposium 2004: Remote Sensing of the Atmosphere, Ocean, Environment, and Space. International Society for Optics and Photonics, 2004. [4] Jaross, G., et al. Initial results from the Ozone Mapper Profiler Suite on the Suomi National Polar-Orbiting Partnership. Geoscience and Remote Sensing Symposium (IGARSS), 2012 IEEE International. IEEE, 2012. [5] Jaross, Glen, et al. Suomi NPP OMPS Limb Profiler initial sensor performance assessment. SPIE Asia-Pacific Remote Sensing. International Society for Optics and Photonics, 2012. ACKNOWLEDGEMENTS: This work is funded under a contract to Ball Aerospace from NASA. The authors wish to thank and congratulate all NASA, NOAA, and Ball Aerospace contributors to OMPS, who helped make it a successful sensor