First light demonstration of the integrated superconducting spectrometer

The coldest and densest structures of gas and dust in the Universe have unique spectral signatures across the (sub-)millimetre bands (ν ≈ 30 − 950 GHz). The current generation of single dish facilities has given a glimpse of the potential for discovery, while sub-mm interferometers have presented a high resolution view into the finer details of known targets or in small-area deep fields. However, significant advances in our understanding of such cold and dense structures are now hampered by the limited sensitivity and angular resolution of our sub-mm view of the Universe at larger scales. In this context, we present the case for a new transformational astronomical facility in the 2030s, the Atacama Large Aperture Submillimetre Telescope (AtLAST). AtLAST is a concept for a 50-m-class single dish telescope, with a high throughput provided by a 2 deg -diameter Field of View, located on a high, dry site in the Atacama with good atmospheric transmission up to ν ∼ 1 THz, and fully powered by renewable energy. We envision AtLAST as a facility operated by an international partnership with a

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“…Example instrumental pathfinders are now abundant in the literature. [59][60][61][62][63][64][65][66][67][68]…”

Section: Proposed Instrumentationmentioning

confidence: 99%

The Atacama large aperture submillimeter telescope (AtLAST) concept

Klaassen

Mroczkowski²,

Bryan

et al. 2020

Ground-Based and Airborne Telescopes VIII

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“…Thus, this would not be a dominant component of photometric errors. in many channels could be attributed to additional offset of input power to the detector, for example, optical coupling to the cold stages in the cryostat, or spillover of the warm optics components caused by optical misalignment between cold and warm optics 2,5 .…”

Section: Resultsmentioning

confidence: 99%

“…In October and November, 2017, we had a first on-sky demonstration of the instrument, covering 332-377 GHz with 49 spectral channels (ν/∆ ν ∼ 380) using the Atacama Submillimeter Telescope Experiment 10-m telescope (ASTE) operated in the Atacama desert, Chile 3,4 . In this session, we successfully detected some astronomical targets, for instance, a redshifted CO(J =3-2) line of VV 114, a luminous infrared galaxy at the redshift of 0.020 5 .…”

Section: Introductionmentioning

confidence: 99%

DESHIMA on ASTE: On-Sky Responsivity Calibration of the Integrated Superconducting Spectrometer

et al. 2020

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We are developing an ultra-wideband spectroscopic instrument, DESHIMA (DEep Spectroscopic HIgh-redshift MApper), based on the technologies of an on-chip filter-bank and Microwave Kinetic Inductance Detector (MKID) to investigate dusty star-burst galaxies in the distant universe at millimeter and submillimeter wavelength. An on-site experiment of DESHIMA was performed using the ASTE 10-m telescope. We established a responsivity model that converts frequency responses of the MKIDs to line-of-sight brightness temperature. We estimated two parameters of the responsivity model using a set of skydip data taken under various precipitable water vapor (PWV, 0.4-3.0 mm) conditions for each MKID. The line-of-sight brightness temperature of sky is estimated using an atmospheric transmission model and the PWVs. As a result, we obtain an average temperature calibration uncertainty of 1σ = 4%, which is smaller than other photometric biases. In addition, the average forward efficiency of 0.88 in our responsivity model is consistent with the value expected from the geometrical support structure of the telescope. We also estimate line-of-sight PWVs of each skydip observation using the frequency response of MKIDs, and confirm the consistency with PWVs reported by the Atacama Large Millimeter/submillimeter Array.

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“…This technique opens up the possibility that future direct detector instruments can be characterized to the quality previously implemented as for heterodyne spectrometer missions, such as Herschel HIFI (see 7 ). This paper overviews the techniques in detail used recently by some of the authors to explain the on sky beam pattern and coupling efficiency for the MKID on-chip spectrometer DESHIMA 23 . For analyzing more complicated optical systems, the measured complex beam patterns could be alternatively be fully propagated, for example in commercial optics software.…”

Section: Discussionmentioning

confidence: 99%

Complex Beam Mapping and Fourier Optics Analysis of a Wide-Field Microwave Kinetic Inductance Detector Camera

et al. 2020

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For astronomical instruments, accurate knowledge of the optical pointing and coupling are essential to characterize the alignment and performance of (sub-)systems prior to integration and deployment. Ideally, this requires the phase response of the optical system, which for direct (phase insensitive) detectors was not previously accessible. Here we show development of the phase sensitive complex beam pattern technique using a dual optical source heterodyne technique for a large field of view Microwave Kinetic Inductance Detector camera at 350 GHz. We show here how you can analyze the measured data with Fourier optics, which allows integration into a telescope model to calculate the on sky beam pattern and telescope aperture efficiency prior to deployment at a telescope.

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First light demonstration of the integrated superconducting spectrometer

Cited by 47 publications

References 37 publications

The Atacama large aperture submillimeter telescope (AtLAST) concept

The Atacama large aperture submillimeter telescope (AtLAST) concept

DESHIMA on ASTE: On-Sky Responsivity Calibration of the Integrated Superconducting Spectrometer

Complex Beam Mapping and Fourier Optics Analysis of a Wide-Field Microwave Kinetic Inductance Detector Camera

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