The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μ m Imaging Atlas of Active Galactic Nuclei Using SOFIA
The Astrophysical Journal: Supplement Series American Astronomical Society 276:2 (2025) 64
Abstract:
We present a 19.7–214 μm imaging atlas of local (4–181 Mpc; median 43 Mpc) active galactic nuclei (AGN) observed with FORCAST and HAWC+ on board the SOFIA telescope with angular resolutions ~3″–20″. This atlas comprises 22 Seyferts (17 Type 2 and five Type 1) with a total of 69 images, 41 of which have not been previously published. The AGN span a range of luminosities of log10(Lbol[ergs-1])=[42, 46] with a median of log10(Lbol[ergs−1])=44.1±1.0 . We provide the total fluxes of our sample using aperture photometry for point-source objects and a 2D Gaussian fitting for objects with extended host galaxy emission, which was used to estimate the unresolved nuclear component. Most galaxies in our sample are pointlike sources; however, four sources (Centaurus A, Circinus, NGC 1068, and NGC 4388) show extended emission in all wavelengths. The 30–40 μm extended emission in NGC 4388 is coincident with the narrow-line region at PA ~ 50°, while the dusty extension at longer wavelengths arises from the host galaxy at PA ~ 90°. Our new observations allow us to construct the best-sampled parsec-scales (spectral energy distributions, SEDs) available between 30 and 500 μm for a sample of nearby AGN. We estimate that the average peak wavelength of the nuclear SEDs is ~40 μm in νFν, which we associate with an unresolved extended dusty region heated by the AGN.JWST Discovery of a Very Fast Biconical Outflow of Warm Molecular Gas in the Nearby Ultraluminous Infrared Galaxy F08572+3915 NW
The Astrophysical Journal American Astronomical Society 979:1 (2025) 68
Bayesian calibration of quasi-static field distortions in HARMONI
RAS Techniques and Instruments Oxford University Press 3:1 (2024) 108-124
Abstract:
The high angular resolution monolithic optical and near-infrared Integral field spectrograph is the first light visible and near-infrared integral field spectrograph for the Extremely Large Telescope. To reach the diffraction limit of the telescope (≈ 10 mas) and maintain an optimal image quality over long exposures, an accurate measurement of geometrical distortions in the instrument’s guide star field is needed. Geometrical distortions affecting the guide stars map directly to pointing errors of the science field. The systematic contribution to the pointing error can be calibrated and removed by a corrective model. In this work, we propose a formulation of the corrective model that aims to calibrate the geometrical field distortions down to a given target residual, as well as reducing the time spent in calibrations. We also propose a calibration procedure that accounts for the uncertainties of the measurement process. We developed a tool named harmoni-pm to simulate the expected pointing error caused by geometrical distortions and validate the effectiveness of the proposed corrective model. We also relied on pseudo Zernike polynomials to formulate the model, and the Bayesian theoretical framework to study the propagation of uncertainties along the calibration process. Compared with the classical calibration algorithm, the Bayesian calibration algorithm was able to reduce the number of calibration points required to reach the same model residual. Additionally, we were able to optimize the hardware of the Geometrical Calibration Unit and reduce the time required to achieve the calibration goal.A Complete 16 μm Selected Galaxy Sample at z ∼ 1: Mid-infrared Spectral Energy Distributions
The Astrophysical Journal American Astronomical Society 912:2 (2021) 161
Predicting the observability of population III stars with ELT-HARMONI via the helium 1640 Å emission line
Monthly Notices of the Royal Astronomical Society Oxford University Press 501:4 (2021) 5517-5537