The current STELLA Echelle spectrograph (SES), which records 390nm to 870nm in one shot at a spectral resolution of 55000, will be replaced by a suite of specialized spectrographs in three spectral bands. The UV will be covered by a newly designed H&K spectrograph covering 380nm to 470nm (SES-H&K), the visual band (470nm - 690nm) will be covered by SES-VIS, which is a vacuum-stabilized spectrograph designed for high radial-velocity accuracy, and the NIR will be covered by the current SES spectrograph from 690nm to 1050nm. In order to improve the UV transmission, and to accommodate three different fibre-feeds, the prime focus corrector of the telescope will be refurbished, leading to an optical system with the f/2 1200mm spherical primary, a 4-lens collimator with 2 arcsec aperture, atmospheric dispersion corrector (ADC), and two dichroic beam splitters, feeding 3 separate fibre feeds for the three bands. The newly designed H&K spectrograph will be an Echelle spectrograph, based on a R4-grating with 41.6 l/mm and 110mmx420mm, using a f/5 camera and the cross-disperser in double pass (as in TRAFICOS, MIKE, KPF), using 21 spectral orders. The spectral resolution of all three spectrographs will be comparable to the 55000 of the current SES.
The \oarpaf telescope is an $80\rm cm$-diameter optical telescope installed in the Antola Mount Regional Reserve, in Northern Italy. This work presents the results of the characterization of the site, as well as developments and interventions that have been implemented, with the goal of exploiting the facility for scientific and educational purposes. During the characterization of the site, an average background brightness of $22.40 \, m_{AB}$ ($B$ filter) -- $21.14 \, m_{AB}$ ($I$) per arcsecond squared, and a $1.5$--$3.0"$ seeing, have been measured. An estimate of the magnitude zero points …
The new SAI MSU observatory 2.5-meter telescope and capabilities of its current instrumentation are described. The facility operates actively since 2014 in parallel to the engineering works. It has delivered a number of prominent results in the field of optical and near-infrared photometry and spectroscopy as well as newly developed observational techniques like differential speckle polarimetry.
Progress in stellar precise radial velocity work will require the stellar, exoplanetary, and instrument scientists in the precise RV community to be better engaged with the heliophysics community. This engagement will require funding for close collaboration among statisticians, heliophysicists, instrument builders, and stellar astronomers, dedicated meetings where the communities can learn about each other and interact inperson, and computational and observational resources to generate the appropriate synthetic and real data sets to drive and prove theoretical understanding of RV jitter.
In 2018-2019 the VERITAS VHE gamma-ray observatory was augmented with highspeed optical instrumentation and continuous data recording electronics to create a sensitive Stellar Intensity Interferometry (SII) observatory, VERITAS-SII. The primary science goal of VERITAS-SII is to perform stellar diameter measurements and image analysis in the visible wavebands on a selection of bright (m< 6), hot (O/B/A) stars. The VERITAS Collaboration has agreed to the deployment and operation of VERITAS-SII during several days each month around the full moon period when VERITAS does not perform VHE gamma-ray …
While observations of many high-precision radio pulsars of order $\lesssim1~μ$s across the sky are needed for the detection and characterization of a stochastic background of low-frequency gravitational waves (GWs), sensitivity to single sources of GWs requires even higher timing precision. The Argentine Institute of Radio Astronomy (IAR; Instituto Argentino de Radioastronomía) has begun observations of the brightest-known millisecond pulsar, J0437$-$4715. Even though the two antennas are smaller than other single-dish telescopes previously used for pulsar timing array (PTA) science, the IAR's…
The IceCube Neutrino Observatory opened the window on neutrino astronomy by discovering high-energy astrophysical neutrinos in 2013 and identifying the first compelling astrophysical neutrino source, the blazar TXS0506+056, in 2017. In this talk, we will discuss the science reach and ongoing development of the IceCube-Gen2 facility---a planned extension to IceCube. IceCube-Gen2 will increase the rate of observed cosmic neutrinos by an order of magnitude, be able to detect five-times fainter neutrino sources, and extend the measurement of astrophysical neutrinos several orders of magnitude high…
The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) over angular scales between 1 arcminute and tens of degrees using over 60,000 detectors and sampling frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 30,000 detectors and an array of half-meter aperture refractive cameras, coupled to an additional 30,000+ detectors. The unique combination of large and small apertures in a single CMB observatory will allow us to sample a wide range of angular scales over a common …
The Canada France Hawaii Telescope Corporation (CFHT) plans to repurpose its observatory on the summit of Maunakea and operate a new wide field spectroscopic survey telescope, the Maunakea Spectroscopic Explorer (MSE). MSE will upgrade the observatory with a larger 11.25m aperture telescope and equip it with dedicated instrumentation to capitalize on the site, which has some of the best seeing in the northern hemisphere, and offer its user community the ability to do transformative science. The knowledge and experience of the current CFHT staff will contribute greatly to the engineering of thi…
We present the Strategic Scientific Plan (SSP) for the direction and activities of the Gemini Observatory in the 2020s. The overarching goal is to ensure that Gemini best uses the available resources to serve the needs of its international user community throughout the coming decade. The actionable items fall into three general categories: (1) preserving Gemini's current facilities and strengths; (2) developing instrumentation and software systems, including data pipelines, to enable new scientific capabilities that build on those strengths; (3) strategizing how visiting instruments can delive…
Goals and strategies in the global control design of the OAJ Robotic Observatory
有很多方法可以解决从头开始制造高性能机器人天文台的挑战性问题。Javalambre天文台（OAJ）是位于Sierra de Javalambre（西班牙特鲁埃尔）的一个新的天文设施，其主要作用是进行全天天文观测。OAJ控制系统是从全局的角度设计的，不仅包括天文子系统，还包括基础设施和其他设施。在机器人OAJ的全局控制系统的设计中考虑了三个主要因素：质量、可靠性和效率。我们建议CIA（控制集成架构）设计和OEE（整体设备效率）作为关键性能指标，以改善操作流程，最大限度地减少资源，并获得高成本降低保持质量要求。控制集成架构考虑的OAJ子系统如下：两台宽视场望远镜及其仪器、主动光学子系统、天空质量监测设施（视宁度，消光，天空背景，天空亮度，云层分布，气象站），圆顶和几个基础设施，如供水，乙二醇水，水处理厂，空调，压缩空气，液氮厂，照明、监视、访问控制、灭火、发电机、配电、电力消耗、通信网络、不间断电源和两个主控制室，一个位于OAJ，另一个位于距天文台40公里的Teruel，通过微波无线电链路连接。在这里，我们提出了OAJ战略控制设计，以实现最大的质量效率的观测过程和操作，给出我们的方法的实际例子。
The IceCube Neutrino Observatory at the South Pole is a multi-component particle detector consisting of the IceTop surface array and the deep in-ice IceCube array. The foreseen enhancement of the surface instrumentation will consist of plastic scintillator panels read out by silicon photomultipliers. This additional detector component will calibrate the effect of snow accumulation on the IceTop tanks, improve the measurement of cosmic rays, and enhance the atmospheric background rejection for the high-energy astrophysical neutrino detection. Two scintillator prototype stations were deployed at…
Mapping Stellar Heterogeneities with the Nautilus Space Observatory
Michigan State University（密歇根州立大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Massachusetts Institute of Technology（麻省理工学院）；Max Planck Institute for Solar System Research（马克斯·普朗克太阳系统研究所）；The University of Arizona（亚利桑那大学）；NASA ICAR/NExSS（美国国家航空航天局 ICAR/NExSS）
The Orbiting Astronomical Satellite for Investigating Stellar Systems (OASIS) is a NASA Astrophysics MIDEX-class mission concept, with the stated goal of following water from galaxies, through protostellar systems, to Earth's oceans. This paper details the protoplanetary disk science achievable with OASIS. OASIS's suite of heterodyne receivers allow for simultaneous, high spectral resolution observations of water emission lines spanning a large range of physical conditions within protoplanetary disks. These observations will allow us to map the spatial distribution of water vapor in disks acro…
Vera C. Rubin Observatory, through the Legacy Survey of Space and Time (LSST), will allow us to derive a panchromatic view of variability in young stellar objects (YSOs) across all relevant timescales. Indeed, both short-term variability (on timescales of hours to days) and long-term variability (months to years), predominantly driven by the dynamics of accretion processes in disk-hosting YSOs, can be explored by taking advantage of the multi-band filters option available in Rubin LSST, in particular the $u,g,r,i$ filters that enable us to discriminate between photospheric stellar properties a…
The Cerro Chajnantor Atacama Telescope-prime (CCAT-prime) is a new 6-m, off-axis, low-emissivity, large field-of-view submillimeter telescope scheduled for first light in the last quarter of 2021. In summary, (a) CCAT-prime uniquely combines a large field-of-view (up to 8-deg), low emissivity telescope (< 2%) and excellent atmospheric transmission (5600-m site) to achieve unprecedented survey capability in the submillimeter. (b) Over five years, CCAT-prime first generation science will address the physics of star formation, galaxy evolution, and galaxy cluster formation; probe the re-ionizatio…
