研究目的
Investigating the temporal and spatial stability of airglow in the Meinel band window at 1191.3 nm to assess the feasibility of ground-based near-infrared line intensity mapping.
研究成果
The airglow at 1191.3 nm is stable in time and space over the observed period, with no evidence of excess noise from atmospheric variations. The measured sky brightness agrees with previous studies, suggesting that ground-based narrowband imaging in near-infrared windows is feasible for detecting diffuse astronomical emissions, though further improvements in sensitivity and systematic control are necessary.
研究不足
The study is limited by the integration time (3.5 hours of stable data), which may not be sufficient to detect very low-level astronomical emissions. Systematic uncertainties from dark current and flat-field corrections affect power spectral measurements, particularly at low spatial frequencies. The instrument's noise is read-noise dominated, and the pointing accuracy and PSF width could be improved. The source of the inter-line continuum remains unidentified, and longer observations are needed to confirm stability over extended periods.
1：Experimental Design and Method Selection:
The study uses a custom-built near-infrared instrument (LAMP) with a λ/Δλ = 320 bandpass centered at 1191.3 nm to measure atmospheric brightness fluctuations. Data were collected over a night from Table Mountain Observatory, with analysis focusing on sky brightness, noise properties, and spatial power spectra.
2：3 nm to measure atmospheric brightness fluctuations. Data were collected over a night from Table Mountain Observatory, with analysis focusing on sky brightness, noise properties, and spatial power spectra.
Sample Selection and Data Sources:
2. Sample Selection and Data Sources: Observations were made of the SWIRE-Lockman Hole field at low airmasses (<1.4) during astronomically dark periods. Data included 245 on-sky integrations, with 91 stable integrations used for detailed analysis.
3：4) during astronomically dark periods. Data included 245 on-sky integrations, with 91 stable integrations used for detailed analysis.
List of Experimental Equipment and Materials:
3. List of Experimental Equipment and Materials: Equipment includes a commercial 10-inch Newtonian telescope, a cryogenic camera with a HAWAII-1 HgCdTe detector array, optical filters (narrowband and blocking filters), and readout electronics. Specific components are detailed in the paper with manufacturers and part numbers.
4：Experimental Procedures and Operational Workflow:
The instrument was mounted on a larger telescope for pointing and tracking. Data were collected in 104 s integrations, with dark and flat-field calibrations performed. Images were processed to subtract dark current, apply flat-field corrections, and perform astrometric registration and masking of sources.
5：Data Analysis Methods:
Analysis involved calculating mean sky brightness, noise rms from image differences, and spatial power spectra using the MASTER formalism. Statistical methods included fitting linear models to detector reads and computing correlation coefficients and χ2 tests for noise consistency.
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