Terahertz atmospheric windows for high angular resolution terahertz astronomy from Dome A
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摘要
Atmospheric transmission from Dome A, Antarctica, presents new possibilities in the field of terahertz astronomy, where space telescopes have been the only observational tools until now. Using atmospheric transmission measurements from Dome A with a Fourier transform spectrometer, transmission spectra and long-term stabilities have been analyzed at 1.461 THz, 3.393 THz, 5.786 THz and 7.1 THz, which show that important atmospheric windows for terahertz astronomy open for a reasonable length of time in the winter season. With large aperture terahertz telescopes and interferometers at Dome A, high angular resolution terahertz observations are foreseen of atomic fine-structure lines from ionized gas and a water ice feature from protoplanetary disks.
Atmospheric transmission from Dome A, Antarctica, presents new possibilities in the field of terahertz astronomy, where space telescopes have been the only observational tools until now. Using atmospheric transmission measurements from Dome A with a Fourier transform spectrometer, transmission spectra and long-term stabilities have been analyzed at 1.461 THz, 3.393 THz, 5.786 THz and 7.1 THz, which show that important atmospheric windows for terahertz astronomy open for a reasonable length of time in the winter season. With large aperture terahertz telescopes and interferometers at Dome A, high angular resolution terahertz observations are foreseen of atomic fine-structure lines from ionized gas and a water ice feature from protoplanetary disks.
Atmospheric transmission from Dome A, Antarctica, presents new possibilities in the field of terahertz astronomy, where space telescopes have been the only observational tools until now. Using atmospheric transmission measurements from Dome A with a Fourier transform spectrometer, transmission spectra and long-term stabilities have been analyzed at 1.461 THz, 3.393 THz, 5.786 THz and 7.1 THz, which show that important atmospheric windows for terahertz astronomy open for a reasonable length of time in the winter season. With large aperture terahertz telescopes and interferometers at Dome A, high angular resolution terahertz observations are foreseen of atomic fine-structure lines from ionized gas and a water ice feature from protoplanetary disks.
引文
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Paine S,Blundell R,Papa D,et al.2000.A Fourier transform spectrometer for measurement of atmospheric transmission at submillimeter wavelengths.Publ Astron Soc Pac,112:108-118.
Shi S C,Paine S,Yao Q J,et al.2016.Terahertz and far-infrared windows opened at Dome A in Antarctica.Nat Astron,1:0001.
Smith R G,Robinson G,Hyland A R,et al.1994.Molecular ices as temperature indicators for interstellar dust:the 44-and 62-μm lattice features of H2O ice.Mon Not R Astron Soc,271:481-489.
Yang J,Zuo Y-X,Lou Z,et al.2013.Conceptual design studies of the 5m terahertz antenna for Dome A,Antarctica.Research in Astron Astrophys,13:1493-1508.
Zhu Y,Wang L,Yuan X,et al.2014.Kunlun Dark Universe Survey Telescope.Proc SPIE,9145:91450E.
Burton M G.2010.Astronomy in Antarctica.Astron Astrophy Rev,18(4):417-469.
Hanbury-Brown R,Twiss R Q.1956.Correlation between photons in two coherent beams of light.Nature,177:2-29.
Hashimoto T,Laporte N,Mawatari K,et al.2018.The onset of star formation 250 million years after the Big Bang.Nature,557:392-395.
Inoue A K,Tamura Y,Matsuo H,et al.2016.Detection of an oxygen emission line from a high-redshift galaxy in the reionization epoch.Science,352:1559-1562.
Khosropanah P,Zhang W,Hovenier J N,et al.2008.3.4 THz heterodyne receiver using a hot electron bolometer and a distributed feedback quantum cascade laser.J Appl Phys,104:113106.
Malfait K,Waelkens C,Bouwman J,et al.1999.The ISO spectrum of the young star HD 142527.Astron Astrophys,345:181-186.
Martin D H,Puplett E.1970.Polarised interferometric spectrometry for the millimeter and submillimeter spectrum.Infrared Phys,10:105-109.
Matsuo H,Ezawa H.2016.Advantages of photon counting detectors for terahertz astronomy.J Low Temp Phys,184:718-723.
Matsushita S,Matsuo H,Pardo J R,et al.1999.FTS measurements of submillimeter-wave atmospheric opacity at Pampa la Bola II:supra-terahertz windows and model fitting.Publ Astron Soc Japan,51:603-610.
Oberst T E,Parshley S C,Nikola T,et al.2011.A 205μm[NII]map of the Carina Nebula.Astrophy J,739:100.
Paine S,Blundell R,Papa D,et al.2000.A Fourier transform spectrometer for measurement of atmospheric transmission at submillimeter wavelengths.Publ Astron Soc Pac,112:108-118.
Shi S C,Paine S,Yao Q J,et al.2016.Terahertz and far-infrared windows opened at Dome A in Antarctica.Nat Astron,1:0001.
Smith R G,Robinson G,Hyland A R,et al.1994.Molecular ices as temperature indicators for interstellar dust:the 44-and 62-μm lattice features of H2O ice.Mon Not R Astron Soc,271:481-489.
Yang J,Zuo Y-X,Lou Z,et al.2013.Conceptual design studies of the 5m terahertz antenna for Dome A,Antarctica.Research in Astron Astrophys,13:1493-1508.
Zhu Y,Wang L,Yuan X,et al.2014.Kunlun Dark Universe Survey Telescope.Proc SPIE,9145:91450E.