Bright Region Reset: an on-detector strategy for minimizing the impacts of atmospheric emission lines on spectral observations

TL;DR

The paper introduces Bright Region Reset (BRR), a novel detector technique that prevents saturation from atmospheric emission lines in near-infrared spectra, enhancing sky line variability monitoring without losing spectral information.

Contribution

The paper presents the BRR method, a new on-detector strategy that mitigates atmospheric emission line saturation and improves variability tracking in near-infrared spectroscopy.

Findings

BRR prevents saturation of bright atmospheric lines in spectra.

No spectral degradation observed with BRR compared to conventional methods.

BRR enables higher-cadence sky line variability measurements.

Abstract

Observations in the near-infrared using large ground-based telescopes are adversely impacted by bright atmospheric emission lines, particularly the OH Meinel bands. These lines can saturate a moderate-resolution spectrograph on the order of minutes, resulting in information loss at the wavelengths of the lines. OH lines also vary on similar timescales, requiring frequent sky exposures to be able to subtract the sky spectrum from that of the target. In this paper we present a new method, which we call bright region reset (BRR), to prevent the saturation of these lines in near-infrared spectra while simultaneously improving information about their variability. This is accomplished by periodically resetting pixels that contain bright lines on a detector capable of sub-window readout while the rest of the detector continues integrating. This method is demonstrated on the McKellar Spectrograph in the 1.2 m telescope at the Dominion Astrophysical Observatory in Victoria, Canada. Using a Teledyne H2RG detector, we reset the emission lines produced by an arc lamp while still recording their flux. We show no degradation in the resulting spectrum compared to a conventional observing mode. Unlike other OH line mitigation strategies, the BRR method not only avoids loss of information at wavelengths containing the lines, but also provides higher-cadence information on sky line variability, making it a promising technique for implementation at observatories. We advocate demonstrating this method on sky at existing 8--10 m class facilities with near-infrared spectrographs equipped with HxRG detectors in order to test its feasibility for use in sky subtraction schemes for premier modern spectrographs, including the upcoming generation of instruments for the Extremely Large Telescopes.