The Far-Infrared Enhanced Survey Spectrometer (FIRESS) for PRIMA: Approach and Estimated Performance
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| Autores principales: | , , , , , , , , , , , , , , , , , , , , , |
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| Formato: | Preprint |
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2025
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| author | M., C. Bradford Kogut, Alan J. Fixsen, Dale Pontoppidan, Klaus Dowell, C. Darren Glenn, Jason Pagano, Thomas Green, Joseph Foote, Marc McGuire, James Rodger, Michael Calvet, Robert Nguyen, Hien Hailey-Dunsheath, Steve Foote, Logan Kane, Elijah Janssen, Reinier M. J. Meixner, Margaret Pope, Alexandra Bolatto, Alberto Smith, JD |
| author_facet | M., C. Bradford Kogut, Alan J. Fixsen, Dale Pontoppidan, Klaus Dowell, C. Darren Glenn, Jason Pagano, Thomas Green, Joseph Foote, Marc McGuire, James Rodger, Michael Calvet, Robert Nguyen, Hien Hailey-Dunsheath, Steve Foote, Logan Kane, Elijah Janssen, Reinier M. J. Meixner, Margaret Pope, Alexandra Bolatto, Alberto Smith, JD |
| contents | We present the architectural concept for the Far-Infrared Enhanced Survey Spectrometer (FIRESS) for the Probe Mission for far-IR Astrophysics (PRIMA). FIRESS spans the 24--235 micron range with four R ~ 100 slit-fed grating modules, each coupling to a 24 (spatial) by 84 (spectral) pixel array of kinetic inductance detectors (KIDs). All four arrays are read out simultaneously, and a point source of interest can be coupled to two of the four bands at a time. A Fourier transform module can be engaged over a portion of the FIRESS slits to create a high-resolution mode in which the light is intercepted, processed by the interferometer then reinserted into the path to the grating modules for detection. We provide a simulation and description of the technique that will be used to obtain high-resolution spectra. We identify the most important system requirements imposed by the detector system, finding that they are met with the existing design. Finally, we present our performance modeling, including both direct estimates given our current design status, as well as durable guidelines for developing general-observer programs. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_02518 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Far-Infrared Enhanced Survey Spectrometer (FIRESS) for PRIMA: Approach and Estimated Performance M., C. Bradford Kogut, Alan J. Fixsen, Dale Pontoppidan, Klaus Dowell, C. Darren Glenn, Jason Pagano, Thomas Green, Joseph Foote, Marc McGuire, James Rodger, Michael Calvet, Robert Nguyen, Hien Hailey-Dunsheath, Steve Foote, Logan Kane, Elijah Janssen, Reinier M. J. Meixner, Margaret Pope, Alexandra Bolatto, Alberto Smith, JD Instrumentation and Methods for Astrophysics Astrophysics of Galaxies Instrumentation and Detectors We present the architectural concept for the Far-Infrared Enhanced Survey Spectrometer (FIRESS) for the Probe Mission for far-IR Astrophysics (PRIMA). FIRESS spans the 24--235 micron range with four R ~ 100 slit-fed grating modules, each coupling to a 24 (spatial) by 84 (spectral) pixel array of kinetic inductance detectors (KIDs). All four arrays are read out simultaneously, and a point source of interest can be coupled to two of the four bands at a time. A Fourier transform module can be engaged over a portion of the FIRESS slits to create a high-resolution mode in which the light is intercepted, processed by the interferometer then reinserted into the path to the grating modules for detection. We provide a simulation and description of the technique that will be used to obtain high-resolution spectra. We identify the most important system requirements imposed by the detector system, finding that they are met with the existing design. Finally, we present our performance modeling, including both direct estimates given our current design status, as well as durable guidelines for developing general-observer programs. |
| title | The Far-Infrared Enhanced Survey Spectrometer (FIRESS) for PRIMA: Approach and Estimated Performance |
| topic | Instrumentation and Methods for Astrophysics Astrophysics of Galaxies Instrumentation and Detectors |
| url | https://arxiv.org/abs/2509.02518 |