AO Assisted Spectroscopy with SINFONI: PSF, Background, and Interpolation

Davies, Richard

doi:10.1007/978-3-540-76963-7_35

Cited by 2 publications

(3 citation statements)

References 20 publications

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“…Moreover, an accurate description of the PSF is required to compare the observations with the model predictions. Since there are no point sources in the field‐of‐view (stars or AGN sources such as nuclei or jet knots), the only way to estimate the achieved PSF is to compare the reconstructed NIFS images with images of higher resolution: those obtained with the HST (for a list of various methods to estimate the PSF see Davies 2007). We first convolve the HST image with a concentric and circular double Gaussian description of the PSF, parametrized as the dispersions of the two components and their relative weight.…”

Section: Determination Of the Point Spread Functionmentioning

confidence: 99%

Determination of masses of the central black holes in NGC 524 and 2549 using laser guide star adaptive optics

Krajnović

McDermid

Cappellari

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We present observations of early‐type galaxies NGC 524 and 2549 with laser guide star adaptive optics (LGS AO) obtained at GEMINI North telescope using the Near‐infrared Integral Field Spectrograph (NIFS) integral field unit (IFU) in the K band. The purpose of these observations is to determine high spatial resolution stellar kinematics within the nuclei of these galaxies and, in combination with previously obtained large‐scale observations with the SAURON IFU, to determine the masses (M•) of the supermassive black holes (SMBH). The targeted galaxies were chosen to have central light profiles showing a core (NGC 524) and a cusp (NGC 2549), to probe the feasibility of using the galaxy centre as the natural guide source required for LGS AO. We employ an innovative technique where the focus compensation due to the changing distance to the sodium layer is made ‘open loop’, allowing the extended galaxy nucleus to be used only for tip‐tilt correction. The data have spatial resolution of 0.23 and 0.17 arcsec full‐width at half maximum (FWHM), where at least ∼40 per cent of flux comes within 0.2, showing that high quality LGS AO observations of these objects are possible. The achieved signal‐to‐noise ratio (S/N ∼ 50) is sufficiently high to reliably determine the shape of the line‐of‐sight velocity distribution. We construct axisymmetric three‐integral dynamical models which are constrained with both the NIFS and SAURON data. The best‐fitting models yield M•= (8.3+2.7−1.3) × 108 M⊙ and (M/L)I= 5.8 ± 0.4 for NGC 524 and M•= (1.4+0.2−1.3) × 107 M⊙ and (M/L)R= 4.7 ± 0.2 for NGC 2549 (all errors are at the 3σ level). We demonstrate that the wide‐field SAURON data play a crucial role in the M/L determination increasing the accuracy of M/L by a factor of at least 5, and constraining the upper limits on black hole masses. The NIFS data are crucial in constraining the lower limits of M• and in combination with the large‐scale data reducing the uncertainty by a factor of 2 or more. We find that the orbital structure of NGC 524 shows significant tangential anisotropy, while at larger radii both galaxies are consistent with having almost perfectly oblate velocity ellipsoids. Tangential anisotropy in NGC 524 coincides with the size of SMBH sphere of influence and the core region in the light profile. This agrees with predictions from numerical simulations where core profiles are the result of SMBH binaries evacuating the centre nuclear regions following a galaxy merger. However, being a disc dominated fast rotating galaxy, NGC 524 has probably undergone through a more complex evolution. We test the accuracy to which M• can be measured using seeings obtained from typical LGS AO observations, and conclude that for a typical conditions and M• the expected uncertainty is of the order of 50 per cent.

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Section: Determination Of the Point Spread Functionmentioning

confidence: 99%

Determination of masses of the central black holes in NGC 524 and 2549 using laser guide star adaptive optics

Krajnović

McDermid

Cappellari

et al. 2009

Monthly Notices of the Royal Astronomical Society

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“…The H4RG‐15 was first adopted for use by the Subaru Prime Focus Spectrograph (Takada 2014; Tamura et al 2022) and the Canada‐France‐Hawaii Telescope SPIRou spectropolarimeter (Donati et al 2018). The H4RG‐15 is now being delivered to European Southern Observatory (ESO) for the MICADO (Davies et al 2021) and HARMONI (Thatte et al 2021) instruments of ESO's ELT. The H4RG‐15 is also operating on the International Space Station in the PIANO (https://digitalcommons.usu.edu/calcon/CALCON2021/all2021content/27/) instrument developed by the Aerospace Corporation.…”

Section: Roics For Infrared Astronomymentioning

confidence: 99%

“…To achieve the desired scientific performance, the mirror shape and phasing needs to be maintained to tens of nm across the entire 39‐m diameter. ESO is developing three first light instruments that use Teledyne's IR FPAs (see Figure 24): MICADO (Davies et al 2021) Adaptive Optics Imaging Camera Nine H4RG‐15 SWIR (2.5

μ

λ_{c o}

) FPAs HARMONI (Thatte et al 2021) Near Infrared Integral Field Spectrograph Eight H4RG‐15 SWIR (2.5

μ

λ_{c o}

) FPAs METIS (Brandl et al, 2021) Imager and Spectrograph One GeoSnap‐18 2K

\times

2K VLWIR (14.5

μ

λ_{c o}

) FPA (described in the next section)Four H2RG MWIR (5.3

μ

λ_{c o}

) FPAs …”

Section: European Southern Observatory Extremely Large Telescopementioning

confidence: 99%

Teledyne imaging sensors' recent contributions to astronomy, earth science, and planetary science

Beletic,

Auyeung,

Pan

et al. 2023

Astron Nachr

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Teledyne Imaging Sensors (TIS) is the leading supplier of infrared focal plane arrays (FPAs) to astronomy and TIS plays a strong role in providing image sensors for Earth and Planetary Science. This article starts with a brief introduction to TIS' technologies and image sensor products. We then present some of TIS' deliveries to space missions and ground‐based telescopes. The space missions include ESA's Euclid Dark Universe mission and several NASA missions (James Webb Space Telescope, Roman Space Telescope, SPHEREx, EMIT). TIS continues to serve ground‐based astronomy by providing the H2RG and the world's largest high‐performance infrared astronomy FPA, the H4RG‐15, to several ground‐based observatories. Active programs will be described. Ongoing work includes NASA's NEO Surveyor asteroid surveillance mission, ESA's Ariel exo‐planet spectroscopy mission, and deliveries to the European Southern Observatory's Extremely Large Telescope.

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AO Assisted Spectroscopy with SINFONI: PSF, Background, and Interpolation

Cited by 2 publications

References 20 publications

Determination of masses of the central black holes in NGC 524 and 2549 using laser guide star adaptive optics

Determination of masses of the central black holes in NGC 524 and 2549 using laser guide star adaptive optics

Teledyne imaging sensors' recent contributions to astronomy, earth science, and planetary science

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