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ATLAS probe: Breakthrough science of galaxy evolution, cosmology, Milky Way, and the Solar System
- Yun Wang, Massimo Robberto, Mark Dickinson, Lynne A. Hillenbrand, Wesley Fraser, Peter Behroozi, Jarle Brinchmann, Chia-Hsun Chuang, Andrea Cimatti, Robert Content, Emanuele Daddi, Henry C. Ferguson, Christopher Hirata, Michael J. Hudson, J. Davy Kirkpatrick, Alvaro Orsi, Russell Ryan, Alice Shapley, Mario Ballardini, Robert Barkhouser, James Bartlett, Robert Benjamin, Ranga Chary, Charlie Conroy, Megan Donahue, Olivier Doré, Peter Eisenhardt, Karl Glazebrook, George Helou, Sangeeta Malhotra, Lauro Moscardini, Jeffrey A. Newman, Zoran Ninkov, Michael Ressler, James Rhoads, Jason Rhodes, Daniel Scolnic, Stephen Smee, Francesco Valentino, Risa H. Wechsler
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- Journal:
- Publications of the Astronomical Society of Australia / Volume 36 / 2019
- Published online by Cambridge University Press:
- 08 April 2019, e015
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- Article
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Astrophysics Telescope for Large Area Spectroscopy Probe is a concept for a National Aeronautics and Space Administration probe-class space mission that will achieve ground-breaking science in the fields of galaxy evolution, cosmology, Milky Way, and the Solar System. It is the follow-up space mission to Wide Field Infrared Survey Telescope (WFIRST), boosting its scientific return by obtaining deep 1–4 μm slit spectroscopy for ∼70% of all galaxies imaged by the ∼2 000 deg2 WFIRST High Latitude Survey at z > 0.5. Astrophysics Telescope for Large Area Spectroscopy will measure accurate and precise redshifts for ∼200 M galaxies out to z < 7, and deliver spectra that enable a wide range of diagnostic studies of the physical properties of galaxies over most of cosmic history. Astrophysics Telescope for Large Area Spectroscopy Probe and WFIRST together will produce a 3D map of the Universe over 2 000 deg2, the definitive data sets for studying galaxy evolution, probing dark matter, dark energy and modifications of General Relativity, and quantifying the 3D structure and stellar content of the Milky Way. Astrophysics Telescope for Large Area Spectroscopy Probe science spans four broad categories: (1) Revolutionising galaxy evolution studies by tracing the relation between galaxies and dark matter from galaxy groups to cosmic voids and filaments, from the epoch of reionisation through the peak era of galaxy assembly; (2) Opening a new window into the dark Universe by weighing the dark matter filaments using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of General Relativity using galaxy clustering; (3) Probing the Milky Way’s dust-enshrouded regions, reaching the far side of our Galaxy; and (4) Exploring the formation history of the outer Solar System by characterising Kuiper Belt Objects. Astrophysics Telescope for Large Area Spectroscopy Probe is a 1.5 m telescope with a field of view of 0.4 deg2, and uses digital micro-mirror devices as slit selectors. It has a spectroscopic resolution of R = 1 000, and a wavelength range of 1–4 μm. The lack of slit spectroscopy from space over a wide field of view is the obvious gap in current and planned future space missions; Astrophysics Telescope for Large Area Spectroscopy fills this big gap with an unprecedented spectroscopic capability based on digital micro-mirror devices (with an estimated spectroscopic multiplex factor greater than 5 000). Astrophysics Telescope for Large Area Spectroscopy is designed to fit within the National Aeronautics and Space Administration probe-class space mission cost envelope; it has a single instrument, a telescope aperture that allows for a lighter launch vehicle, and mature technology (we have identified a path for digital micro-mirror devices to reach Technology Readiness Level 6 within 2 yr). Astrophysics Telescope for Large Area Spectroscopy Probe will lead to transformative science over the entire range of astrophysics: from galaxy evolution to the dark Universe, from Solar System objects to the dusty regions of the Milky Way.
The HST survey of the Orion Nebula region
- Massimo Robberto
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- Journal:
- Proceedings of the International Astronomical Union / Volume 1 / Issue S227 / May 2005
- Published online by Cambridge University Press:
- 08 November 2005, pp. 358-363
- Print publication:
- May 2005
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The HST Treasury Program on the Orion Nebula Cluster has been recently completed (May 2005). Using 104 orbits of HST time we have imaged a field ${\sim }1/6$ of a square degree nearly centered on the Trapezium stars. The survey, made with ACS, WFPC2 and NICMOS-Camera 3 in parallel, has imaged this cornerstone region with unprecedented sensitivity (23-24 mag), dynamic range (${\sim}12$ mag), spatial resolution (50mas), and wide spectral coverage (9 filters from U to H). We have assembled the richest, most accurate and unbiased dataset of stellar photometry for pre-main-sequence objects ever obtained, an essential tool for understanding of the star formation process in regions dominated by massive OB stars.
S119: a new Luminous Blue Variable?
- from Part two - Wolf-Rayet Ring Nebulae
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- By Antonella Nota, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD; Affiliated to ESA, Astrophysics Division, Space Science Department, of ESA, Laurent Drissen, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, Mark Clampin, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, Claus Leitherer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, Anna Pasquali, Universita' di Firenze, Arcetri, Italy, Carmelle Robert, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, Francesco Paresce, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD; Affiliated to ESA, Astrophysics Division, Space Science Department, of ESA; Universita' di Firenze, Arcetri, Italy, Massimo Robberto, Osservatorio di Torino, Pino Torinese, Italy
- Edited by R. E. S. Clegg, Royal Greenwich Observatory, Cambridge, I. R. Stevens, Imperial College of Science, Technology and Medicine, London, W. P. S. Meikle, University of Birmingham
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- Book:
- Circumstellar Media in Late Stages of Stellar Evolution
- Published online:
- 07 September 2010
- Print publication:
- 25 August 1994, pp 89-94
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Summary
Introduction
The LMC star S119 is a member of the group of Ofpe/WN9 stars listed by Bohannan and Walborn (1989). The Ofpe/WN9 category, first defined by Walborn (1982), identifies peculiar supergiants whose spectra combine the typical Of characteristic emission lines of He II and N III with equally strong lower ionization emission features, such as those of He I and N II, and are believed to represent a transition phase in the evolution between massive O stars and WR stars.
High Resolution Echelle Observations
We have observed S119 with the high resolution echelle spectrograph EMMI, coupled to the NTT, ESO La Silla, on September 18, 1991. The spectra cover the wavelength range 4100Å- 7800Å, with a spectral resolution of 0.089 Å/pixel at 6563 Å. The selected slit width was 1.5″ × 5″, with a plate scale on the detector of 0.345″/pixel. In the spectrum, previously undetected nebular lines of Hα, Hβ, [NII], [SII] appear strong and spatially extended, an indication that S119 is surrounded by a bright gaseous nebula. We detect clear splitting of all the observed nebular lines. In Figure 1 we show the radial velocity map obtained from the [NII] 6583 Å line profile. During the observation the slit was oriented EW, and the star was not centered in the aperture, so that only the eastern portion of the nebula lies completely within the slit, while the western region is marginally covered (≃ 2″).