Image quality is sensitive to temperature fluctuations on the optical path, even if these are not fully developed turbulence. Thus, it’s crucial to control the thermal environment, be it on a test bench in the laboratory, in instruments (e.g., entrance windows, near electronics), within domes and telescope structures. It is especially crucial where the beam is small (i.e., going through a focus) and the power spectrum of the refractive index can be anything from high frequencies to just tip-tilt.
We have used our optical turbulence sensor AIRFLOW to explore how a DT of a few degrees in the optical path can undo a lot of what an AO system can improve, and we are using our devices to study quantitative ways to minimize the image degradation induced by temperature fluctuations. These may include counterintuitive measures such as fans mixing the air at different temperatures, because mechanical turbulence with no DT doesn’t produce optical turbulence.
Maunakea Spectroscopic Explorer (MSE) is a telescope dedicated to multi-fibers spectroscopy and IFUs observations of the sky. Program Execution System Architecture (PESA) is one of the systems of MSE, responsible for planning, executing, reducing, and distributing science products from survey programs. Work is being done to design PESA in a modular way to include several sophisticated software tools, organized into an operational framework. This paper describes the first step of its organization and the concepts that will be used in the development of PESA.
As the crisis of climate change affects more people every year and leads to more severe weather patterns with unprecedented socio-economical consequence, all actors on the planet need to understand their responsibility and contribute to solving this generational problem. To tackle this issue, individuals and corporations first need to assess their carbon footprint, which then represents the groundwork for the future implementation of significant changes required to reduce that footprint. We present the carbon emissions attributed to the Canada–France–Hawaii Telescope (CFHT) for the year 2019. We partnered with CarbonBuddy and followed their method to break down the greenhouse gas (GHG) emissions of various activities at CFHT for the entire year of 2019: air travel in and out of state, ground vehicle usage, electricity consumption, and other fossil fuel utilization. The total GHG emissions of CFHT for the year 2019 amount to about 749 tons of CO2 equivalent, which corresponds to more than 16 tons per employee. About 63% of the emissions are related to electricity usage at the summit facility, about 25% to out-of-state travel, about 6% to the use of our fleet of vehicles, and about 5% to electricity usage at headquarters. We show that significant improvements have occurred in the recent past at CFHT, with the installation of solar panels and a remarkable reduction in electricity consumption at headquarters. We list suggestions to further decrease the GHG emissions in the short to long term: offset current emissions by support local projects, invest in more efficient equipment, and establish environmentally friendly habits. The fundamental work presented will facilitate the official planning at CFHT for a drastic reduction in GHG emissions with the goal to meet the objectives laid out in the 2015 Paris Accord. It will also support the design of the Maunakea Spectroscopic Explorer (MSE), the future transformation of CFHT, and allow the project to seize this opportunity and incorporate the fight against climate change as one of its core missions. By choosing to implement those changes, CFHT and MSE can become part of the solution to climate change and lead the way, locally and in the world of astronomy.
The Maunakea Spectroscopic Explorer (MSE) will transform the Canada-France-Hawaii Telescope into an 11.25-m aperture telescope, dedicated to highly multiplexed, visible to near-IR spectroscopic studies with multiple spectral resolution modes. A metric of MSE’s success is survey speed, i.e. how many scientifically useful spectra MSE will obtain in support of its surveys, which requires hardware and software to be designed and perform efficiently. In this paper, we describe the front-end software, which includes proposal review, a scheduler, an exposure time calculator, and a breaker to prepare and define the survey observations, and the back-end software, which includes data reduction and science pipelines, science archive, and science platform to deliver the data back to the science community. The interfaces, the flow of data, and the overarching object model will be explained. We also discuss the tools required to support the Design Reference Survey that describes and simulates the science operations of MSE.
The Maunakea Spectroscopic Explorer is designed to be the largest non-ELT optical/NIR astronomical telescope, and will be a fully dedicated facility for multi-object spectroscopy over a broad range of spectral resolutions. The MSE design has progressed from feasibility concept into its current baseline design where the system configuration of main systems such as telescope, enclosure, summit facilities and instrument are fully defined. This paper will describe the engineering development of the main systems, and discuss the trade studies to determine the optimal telescope and multiplexing designs and how their findings are incorporated in the current baseline design.
MSE is a wide field telescope (1.5 square degree field of view) with an aperture of 11.25m. It is dedicated to multi-object spectroscopy at several different spectral resolutions in the range R ~ 2500 - 40000 over a broad wavelength range (0:36 - 1:8μm). MSE enables transformational science in areas as diverse as exoplanetary host characterization; stellar monitoring campaigns; tomographic mapping of the interstellar and intergalactic media; the in-situ chemical tagging of the distant Galaxy; connecting galaxies to the large scale structure of the Universe; measuring the mass functions of cold dark matter sub-halos in galaxy and cluster-scale hosts; reverberation mapping of supermassive black holes in quasars. Here, we summarize the Observatory and describe the development of the top level science requirements and operational concepts. Specifically, we describe the definition of the Science Requirements to be the set of capabilities that allow certain high impact science programs to be conducted. We cross reference these science cases to the science requirements to illustrate the traceability of this approach. We further discuss the operations model for MSE and describe the development of the Operations Concept Document, one of the foundational documents for the project. We also discuss the next stage in the science based development of MSE, specifically the development of the initial Legacy Survey that will occupy a majority of time on the telescope over the first few years of operation.
The local turbulence is the only part of the seeing degradation that we can actively improve and reduce at the source. It is often a major contribution to the overall seeing1,2 and introduces effects that are highly localized and may be difficult to correct. For example, dome seeing is expected to be non-Kolmogorov, with a very small outer scale leading to a preponderance of high spatial frequencies. The first step in controlling the local seeing is to locate and quantify the turbulence present. This requires the development of a new type of sensor, specifically designed to sensitively measure local optical turbulence. We are in the process of developing such a sensor, based on a simple Mach-Zehnder interferometer layout. The sensor will be light and ruggedized so that it can be used to map out the turbulence inside the dome of any telescope, inside the telescope tube and even around the dome building. Eventually, such a sensor may be used to quantitatively and actively control dome vents.
The Canada-France-Hawaii Telescope is currently in the conceptual design phase to redevelop its facility into the new Maunakea Spectroscopic Explorer (MSE). MSE is designed to be the largest non-ELT optical/NIR astronomical telescope, and will be a fully dedicated facility for multi-object spectroscopy over a broad range of spectral resolutions. This paper outlines the software and control architecture envisioned for the new facility. The architecture will be designed around much of the existing software infrastructure currently used at CFHT as well as the latest proven opensource software. CFHT plans to minimize risk and development time by leveraging existing technology.
Jean-Charles Cuillandre, Kanoa Withington, Patrick Hudelot, Yuliana Goranova, Henry McCracken, Frédéric Magnard, Yannick Mellier, Nicolas Regnault, Marc Bétoule, Hervé Aussel, J. J. Kavelaars, Pierre Fernique, François Bonnarel, Francois Ochsenbein, Olivier Ilbert
The Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) is a high impact scientific program which will
see its final official release open to the world in 2012. That release will seal the legacy aspect of the survey
which has already produced a large collection of scientific articles with topics ranging from cosmology to the
Solar system. The survey core science was focused on dark energy and dark matter: the full realization of the
scientific potential of the data set gathered between 2003 and 2009 with the MegaCam wide-field imager mounted
at the CFHT prime focus is almost complete with the Supernovae Legacy Survey (SNLS) team preparing its
third and last release (SNLS5), and the CFHTLenS team planning the release based around the cosmic shear
survey later this year. While the data processing center TERAPIX offered to the CFHTLS scientific community
regular releases over the course of the survey in its data acquisition phase (T0001-T0006), the final release took
three years to refine in order to produce a pristine data collection photometrically calibrated at better than the
percent both internally and externally over the total survey surface of 155 square degrees in all five photometric
bands (u*, g’, r’, i’, z’). This final release, called T0007, benefits from the various advances in photometric
calibration MegaCam has benefited through the joint effort between SNLS and CFHT to calibrate MegaCam
at levels unexplored for an optical wide-field imager. T0007 stacks and catalogs produced by TERAPIX will be
made available to the world at CADC while the CDS will offer a full integration of the release in its VO tools
from VizieR to Aladin. The photometric redshifts have been produced to be released in phase with the survey.
This proceeding is a general introduction to the survey and aims at presenting its final release in broad terms.
OPERA is a Canada-France-Hawaii Telescope (CFHT) open source collaborative software project currently under
development for an ESPaDOnS echelle spectro-polarimetric image reduction pipeline. OPERA is designed to be
fully automated, performing calibrations and reduction, producing one-dimensional intensity and polarimetric
spectra. The calibrations are performed on two-dimensional images. Spectra are extracted using an optimal
extraction algorithm. While primarily designed for CFHT ESPaDOnS data, the pipeline is being written to be
extensible to other echelle spectrographs. A primary design goal is to make use of fast, modern object-oriented
technologies. Processing is controlled by a harness, which manages a set of processing modules, that make use
of a collection of native OPERA software libraries and standard external software libraries. The harness and
modules are completely parametrized by site configuration and instrument parameters. The software is open-
ended, permitting users of OPERA to extend the pipeline capabilities. All these features have been designed to
provide a portable infrastructure that facilitates collaborative development, code re-usability and extensibility.
OPERA is free software with support for both GNU/Linux and MacOSX platforms. The pipeline is hosted on
SourceForge under the name "opera-pipeline".
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