scholarly journals Okayama Astrophysical Observatory Wide-Field Camera

2019 ◽  
Vol 71 (6) ◽  
Author(s):  
Kenshi Yanagisawa ◽  
Yasuhiro Shimizu ◽  
Kiichi Okita ◽  
Daisuke Kuroda ◽  
Hironori Tsutsui ◽  
...  
Keyword(s):  
Focal Plane ◽  
Near Infrared ◽  
Galactic Plane ◽  
Focal Plane Array ◽  
Variable Stars ◽  
Field Of View ◽  
Wide Field

Abstract We report on the development of a wide-field near-infrared (0.9–2.5$\, \mu$m) camera built as a renewal of the existing classical Cassegrain 0.91 m telescope at Okayama Astrophysical Observatory. The optics system was replaced with fast hybrid optics (f/2.5) composed of forward Cassegrain optics and quasi-Schmidt optics, which results in an effective image circle of 52 mm diameter on the focal plane. The new camera, called the Okayama Astrophysical Observatory Wide-Field Camera (OAOWFC), has imaging capabilities in the $Y$, $J$, $H$, and $K_{\rm s}$ bands over a field of view of $0.^{\!\!\!\circ }47 \times 0.^{\!\!\!\circ }47$ with a HAWAII-1 HgCdTe PACE focal plane array. The primary purpose of OAOWFC is to search for variability in the Galactic plane in the $K_{\rm s}$ band and to promptly follow up transients. We have demonstrated a photometric repeatability of 2% in the densest field in the northern Galactic plane and successfully discovered previously unreported variable stars. The observations of OAOWFC are fully autonomous, and we started scientific operations in 2015 April.

Wide-field-of-view PtSi infrared focal plane array

1990 ◽  
Author(s):  
Edward T. Nelson ◽  
Kwok Y. Wong ◽  
Shozo Yoshizumi ◽  
D. Rockafellow ◽  
William Des Jardin ◽  
...  
Keyword(s):  
Focal Plane ◽  
Focal Plane Array ◽  
Field Of View ◽  
Wide Field ◽  
Infrared Focal Plane Array ◽  
Wide Field Of View

Optical Design of COLIBRÍ: A Fast Follow-up Telescope for Transient Events

2020 ◽  
Vol 09 (01) ◽  
pp. 2050001 ◽  
Author(s):  
J. Fuentes-Fernández ◽  
A. M. Watson ◽  
S. Cuevas ◽  
S. Basa ◽  
J. Floriot ◽  
...  
Keyword(s):  
Image Quality ◽  
Ambient Temperature ◽  
Focal Plane ◽  
Near Infrared ◽  
Optical Design ◽  
Field Of View ◽  
The Future ◽  
Transient Events

COLIBRÍ will be a Franco-Mexican 1.3-m telescope and imager for observing the visible and near infrared counterparts of transient events detected by the future SVOM mission. The imager is divided into two instruments: DDRAGO, with two 4k[Formula: see text][Formula: see text][Formula: see text]4k CCDs observing in [Formula: see text] and [Formula: see text], respectively, and CAGIRE, with one 2k[Formula: see text][Formula: see text][Formula: see text]2k LYNRED or H2RG detector observing in [Formula: see text]. DDRAGO will directly image the telescope focal plane with a field of view (FoV) of 26[Formula: see text][Formula: see text][Formula: see text]26 arcmin. CAGIRE will reimage the focal plane to make a pupil image available for a cold stop and adjust the plate scale to deliver a similar FoV. CAGIRE will not use a conventional collimator-camera configuration but rather an arrangement of lenses that sends the pupil image close to the focal plane after all of the reimaging optics. This allows most of the optics, including the infrared filters, to be at ambient temperature and avoids the complexity of having mechanisms and powered optics within the cryostat (CR). We present here the optical design of the system and a thorough analysis on the expected image quality of the instruments and the telescope.

Wide field-of-view dual-focal-plane augmented reality display

2019 ◽  
Author(s):  
Ugur Yekta Basak ◽  
Seyedmahdi M. K. Kazempourradi ◽  
Erdem Ulusoy ◽  
Hakan Urey
Keyword(s):  
Augmented Reality ◽  
Focal Plane ◽  
Field Of View ◽  
Wide Field ◽  
Wide Field Of View

scholarly journals ESO Spectroscopic Facility

2017 ◽  
Vol 13 (S334) ◽  
pp. 242-247
Author(s):  
Luca Pasquini ◽  
B. Delabre ◽  
R. S. Ellis ◽  
J. Marrero ◽  
L. Cavaller ◽  
...  
Keyword(s):  
High Resolution ◽  
Wavelength Range ◽  
Focal Plane ◽  
Working Group ◽  
Field Of View ◽  
High Resolution Spectroscopy ◽  
Wide Field ◽  
Low Resolution ◽  
Field Unit ◽  
Integral Field

AbstractWe present the concept of a novel facility dedicated to massively-multiplexed spectroscopy. The telescope has a very wide field Cassegrain focus optimised for fibre feeding. With a Field of View (FoV) of 2.5 degrees diameter and a 11.4m pupil, it will be the largest etendue telescope. The large focal plane can easily host up to 16.000 fibres. In addition, a gravity invariant focus for the central 10 arc-minutes is available to host a giant integral field unit (IFU). The 3 lenses corrector includes an ADC, and has good performance in the 360-1300 nm wavelength range. The top level science requirements were developed by a dedicated ESO working group, and one of the primary cases is high resolution spectroscopy of GAIA stars and, in general, how our Galaxy formed and evolves. The facility will therefore be equipped with both, high and low resolution spectrographs. We stress the importance of developing the telescope and instrument designs simultaneously. The most relevant R&D aspect is also briefly discussed.

Room temperature 640x512 pixel near-infrared InGaAs focal plane array

2000 ◽  
Author(s):  
Martin H. Ettenberg ◽  
Michael J. Lange ◽  
Matthew T. O'Grady ◽  
Jacobus S. Vermaak ◽  
Marshall J. Cohen ◽  
...  
Keyword(s):  
Focal Plane ◽  
Room Temperature ◽  
Near Infrared ◽  
Focal Plane Array

scholarly journals Mapping large-scale diffuse γ-ray emission in the 10−100 TeV band with Cherenkov telescopes

2020 ◽  
Vol 637 ◽  
pp. A44 ◽  
Author(s):  
A. Neronov ◽  
D. Semikoz
Keyword(s):  
Large Scale ◽  
Galactic Plane ◽  
Cosmic Ray ◽  
Field Of View ◽  
Medium Size ◽  
Wide Field ◽  
Galactic Latitude ◽  
Cherenkov Telescopes ◽  
Diffuse Flux ◽  
Astrophysical Neutrino

Context. Measurement of diffuse γ-ray emission from the Milky Way with Imaging Atmospheric Cherenkov Telescopes (IACT) is difficult because of the high level of charged cosmic ray background and the small field of view. Aims. We show that such a measurement is nevertheless possible in the energy band 10−100 TeV. Methods. The minimal charged particle background for IACTs is achieved by selecting the events to be used for the analyses of the cosmic ray electrons. Tight cuts on the event quality in these event selections allow us to obtain a sufficiently low background level to allow measurement of the diffuse Galactic γ-ray flux above 10 TeV. We calculated the sensitivities of different types of IACT arrays for the Galactic diffuse emission measurements and compared them with the diffuse γ-ray flux from different parts of the sky measured by the Fermi Large Area Telescope below 3 TeV and with the astrophysical neutrino signal measured by IceCube telescope. Results. We show that deep exposure of existing IACT systems is sufficient for detection of the diffuse flux from all the Galactic Plane up to Galactic latitude |b| ∼ 5°. The Medium Size Telescope array of the CTA will be able to detect the diffuse flux up 30° Galactic latitude. Its sensitivity will be sufficient for detection of the γ-ray counterpart of the Galactic component of the IceCube astrophysical neutrino signal above 10 TeV. We also propose that a dedicated IACT system composed of small but wide-field-of-view telescopes could be used to map the 10−100 TeV diffuse γ-ray emission from across the whole sky. Conclusions. Detection and detailed study of diffuse Galactic γ-ray emission in the previously unexplored 10−100 TeV energy range is possible with the IACT technique. This is important for identification of the Galactic component of the astrophysical neutrino signal and for understanding the propagation of cosmic rays in the interstellar medium.

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