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Journal articles on the topic 'IUCAA 2 M telescope'

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Author: Grafiati

Published: 18 May 2024

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1

Srivastava, Mudit K., A. N. Ramaprakash, Hillol K. Das, Mahesh P. Burse, Pravin A. Chordia, Abhay A. Kohok, and Chaitanya V. Rajarshi. "Design and development of an optical-fibre-based Integral Field Unit (IFU) on the IUCAA 2-m telescope." Monthly Notices of the Royal Astronomical Society 418, no. 2 (October 20, 2011): 1127–37. http://dx.doi.org/10.1111/j.1365-2966.2011.19560.x.

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2

Anandaram, Mandayam N., B. A. Kagali, and S. P. Bhatnagar. "Design of a Small Automated Telescope for Indian Universities." Transactions of the International Astronomical Union 24, no. 3 (2001): 303–6. http://dx.doi.org/10.1017/s0251107x00000973.

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AbstractWe have constructed a computer controlled telescope using a 0.36-m f/11 Celestron optical tube assembly for teaching and research applications. We have constructed a heavy duty fork-type equatorial mount fitted with precision machined 24 inch drive disks for both axes. These are friction driven by stepper motors through one inch rollers. We have used an open loop control system triggerable by an ST-4 CCD camera to acquire and track any target object. Our telescope can home in on any target within a range of two arc-minutes. We have employed a commercial stepper motor controller card for which we have written a user friendly pc based telescope control software in C. Photometry using a solid state photometer, and imaging by an ST-6 CCD camera are possible.We consider that this project is suitable for those wishing to construct some parts of a telescope and understand the principles of operation. A simpler model of this telescope could use DC motors instead of stepper motors. We shall be happy to send our design diagrams and details to those interested. This project was funded by the DST, and was assisted by IUCAA, Pune.

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3

Geyl, R., and H. Gashut. "A 2-m robotic telescope project." Astronomische Nachrichten 325, no. 6-8 (October 2004): 665–66. http://dx.doi.org/10.1002/asna.200410320.

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4

Takato, N., T. Ichikawa, F. Uraguchi, R. Lundock, C. Murata, Y. Taniguchi, H. Motoyama, K. Fukui, and M. Taguchi. "A 2-m class Telescope at Dome Fuji." EAS Publications Series 33 (2008): 271–74. http://dx.doi.org/10.1051/eas:0833038.

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5

Getov, R. G. "Photographic Surface Photometry of Bright Galaxies in the M 81 Group." Symposium - International Astronomical Union 161 (1994): 594–95. http://dx.doi.org/10.1017/s0074180900048154.

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A programme for the surface photometry of bright galaxies has been underway at the Rozhen Observatory since 1991. In a series of papers we shall explore the optical morphology, photometric properties and some peculiarities suggestive of galaxy-galaxy interactions of the bright galaxies NGC 2976, NGC 3031, NGC 3034 and NGC 3077 in the M 81 group. Most of the plates were taken with the 2 m Rozhen Ritchey-Chrétien telescope, but at our disposal there are plates from the 6 m BTA and 2 m Tautenburg Schmidt telescope. Here we discuss some preliminary results for the optical morphology on the basis of two B-plates from the 2 m Tautenburg Schmidt telescope. It shows the edge-on like face of NGC 2976, the grand-designed spiral structure of NGC 3031 and the filament-jet peculiarities in NGC 3034 and NGC 3077.

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6

Mirzoyan, Razmick. "Status of the 17 m diameter MAGIC telescope." European Physical Journal C 33, S1 (February 3, 2004): s938—s940. http://dx.doi.org/10.1140/epjcd/s2004-03-1630-2.

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7

DENG Yong-ting, 邓永停, 李洪文 LI Hong-wen, 王建立 WANG Jian-li, and 陈. 涛. CHEN Tao. "Main axes AC servo control system for 2 m telescope." Optics and Precision Engineering 25, no. 1 (2017): 163–71. http://dx.doi.org/10.3788/ope.20172501.0163.

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8

Xia Peipei, 夏培培, 邓永停 Deng Yongting, 王志乾 Wang Zhiqian, 李洪文 Li Hongwen, and 王显军 Wang Xianjun. "Model identification for K mirror turntable of 2 m telescope." Infrared and Laser Engineering 47, no. 3 (2018): 318001. http://dx.doi.org/10.3788/irla201847.0318001.

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9

Silva-Cabrera, José Sergio, Joel Humberto Castro-Chacón, Mauricio Reyes-Ruiz, Matthew J. Lehner, Carlos Alberto Guerrero, Chung-Kai Huang, Fernando Iván Alvarez-Santana, et al. "2018 August 15 stellar occultation by minor planet (134340) Pluto." Monthly Notices of the Royal Astronomical Society 511, no. 4 (March 8, 2022): 5550–59. http://dx.doi.org/10.1093/mnras/stac401.

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ABSTRACT We present photometric light curves of the stellar occultation event of the star UCAC4 341-187633 on 2018 August 15 by the minor planet (134340) Pluto. Photometric observations were carried out using the 2.1-m telescope at the San Pedro Mártir Observatory and the 1.3-m telescopes at Sites 2 and 3 of the Trans-Neptunian Automated Occultation Survey (TAOS II) project, and using a portable 0.4-m telescope from Bahía Asunción, Baja California Sur, Mexico. Different filters were used with the 2.1-m telescope and the TAOS II telescopes, whilst observations with the portable system were performed with no filter. The resulting light curves from the San Pedro Mártir Observatory show clear structures, with at least two bright spikes observed on ingress and one more observed on egress as the star traverses the atmosphere of the dwarf planet. The light curve from the portable telescope (440 km away) measured a longer duration for the occultation event, because the shadow of Pluto was observed at a lower latitude. Normalized light curves were created for the 2.1-m telescope, the Site 3 telescope of the TAOS II and the portable telescope. These normalized light curves show a difference in amplitude.

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10

Akabane, Kenji, Shozo Tsunekawa, Makoto Inoue, Ryohei Kawabe, Nagayoshi Ohashi, Osamu Kameya, Masato Ishiguro, and Yoshiaki Sofue. "Millimeter-Wave Continuum Around NGC 7538-IRS1, IRS2, and IRS3." International Astronomical Union Colloquium 140 (1994): 258–59. http://dx.doi.org/10.1017/s0252921100019692.

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Millimeter-wave continuum sources in NGC 7538 region were observed with the NRO 45-m telescope and Nobeyama Millimeter Array. NRO 45-m telescope observations showed that the compact region which includes IRS1, IRS2, and IRS3 has a strong millimeter-wave intensity excess, cf. figures 1, and 2.

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11

Mendoza, E. E., C. Chavarría-K., and V. M. Arévalo. "Narrow Band Photometry and Mapping of the Planetary Nebulae NGC 6210 and NGC 7009." Symposium - International Astronomical Union 131 (1989): 49. http://dx.doi.org/10.1017/s0074180900137489.

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This paper is based upon observations carried out at the Observatorio Astronómico Nacional, San Pedro Mártir, B.C.N. México. They are of two types: (1) α(16)Λ(9)-photometry, obtained with the 1.5-m Johnson telescope, and (2) maps at the wavelengths of Hα and λ7751 A [Ar III] emission lines secured with the 2.1-m telescope.

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12

Pierro, Federico Di. "Status of the Large-Sized Telescope of the Cherenkov Telescope Array." Journal of Physics: Conference Series 2429, no. 1 (February 1, 2023): 012020. http://dx.doi.org/10.1088/1742-6596/2429/1/012020.

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Abstract The Large-Sized Telescopes (LSTs) of the Cherenkov Telescope Array (CTA) are designed for gamma-ray studies focusing on low energy threshold, high flux sensitivity and rapid telescope repositioning. The LST has a tessellated parabolic mirror of 23 m diameter and a weight of about 100 tons, with the capability of pointing to any position in the sky in 20 seconds or less to catch transients. A 2 ton 3x3 m camera, placed in the focus of the mirror, is equipped with 1855 high QE PMTs corresponding to a FoV of about 4.5 degrees. LSTs will dominate the CTA performance between 20 GeV and approximately 200 GeV. The first LST (LST-1) was inaugurated in La Palma (Spain) in October 2018 and since then it is in the commissioning phase. The current status and performance of the LST-1 are discussed. The telescope behavior is well understood and the performance has reached the design level in terms of sensitivity, angular and energy resolutions. Still some work is needed to achieve the duty cycle goal. We briefly present here some of the first physics results. Finally the outlooks of the project are presented.

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13

Gomboc, Andreja, Michael F. Bode, David Carter, Carol G. Mundell, Andrew Newsam, Robert J. Smith, and Iain A. Steele. "The Liverpool Telescope: rapid follow-up observation of targets of opportunity with a 2 m robotic telescope." Nuclear Physics B - Proceedings Supplements 132 (June 2004): 312–15. http://dx.doi.org/10.1016/j.nuclphysbps.2004.04.055.

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14

Borovička, Jiří, and Jaime Zamorano. "The spectrum of fireball light taken with a 2-m telescope." Earth, Moon, and Planets 68, no. 1-3 (January 1995): 217–22. http://dx.doi.org/10.1007/bf00671511.

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15

Eaton, J. A., and M. H. Williamson. "Managing the operations of the TSU 2-m Automatic Spectroscopic Telescope." Astronomische Nachrichten 325, no. 6-8 (October 2004): 522–26. http://dx.doi.org/10.1002/asna.200410272.

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16

Herouni, P. M., and V. S. Oskanian. "Radio flare on η Gemini Star." Symposium - International Astronomical Union 137 (1990): 145–46. http://dx.doi.org/10.1017/s0074180900187613.

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The first at the world Radio-Optical Telescope ROT-32/54/2, 6 was mounted on the southern slope of Mount Aragats in Armenia at 1700 m above sea level. The Large Antenna of ROT with the unmovable hemisperical main mirror of 54 m in diameter and movable small correcting mirror is the extremely accurate and shortwave (down to 1 mm). Using aperture is 32m. The diameter of the Optical Telescope is 2.6 m. General view of ROT is shown in Fig.1.

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17

McGregor, Peter J., Peter Conroy, Jan van Harmelen, and Michael S. Bessell. "A New Acquisition and Autoguiding Camera for the ANU 2·3 m Telescope." Publications of the Astronomical Society of Australia 17, no. 1 (2000): 102–8. http://dx.doi.org/10.1071/as00102.

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AbstractA new, direct CCD acquisition and autoguiding camera is in use on the ANU 2·3 m telescope Nasmyth foci. The camera is a model AP7 manufactured by Apogee Instruments Inc. and is controlled by the MaxIm CCD camera control and image processing software developed by Diffraction Ltd. The factors influencing our choice of this new camera are discussed, and its performance, operation, and commercial control software are described. The new camera allows stellar objects as faint as B = 21·5 to be acquired on the Double Beam Spectrograph slit in 1·4″ seeing. The camera has far superior performance to the Fairchild intensified CCD cameras that it replaces. The improved acquisition and guiding permitted by this camera has already allowed several new scientific programs to begin on the telescope, including the use of aperture plates with the Double Beam Spectrograph.

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18

Stavrev, K. Y., and I. S. Barzova. "Direct-Photography Observations by the 2 M RCC Telescope at Nao-Rozhen: Catalogue of Plates and Archive-Data Analysis." Symposium - International Astronomical Union 161 (1994): 371–75. http://dx.doi.org/10.1017/s0074180900047690.

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The 2m Ritchey-Chrétien-Coudé (RCC) telescope of the National Astronomical Observatory, situated in the Rozhen massif of the Rhodope Mountains, started operating in 1980 (for a detailed description of the telescope see Gutcke [1979]). Since then, 2000 direct photographs have been obtained, most of them covering a 1° × 1° area on the sky with resolution 12.9 sec/mm.

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19

Mazel, Jean, and Robert Futaully. "The “Sonate” Campaign." International Astronomical Union Colloquium 98 (1988): 173–74. http://dx.doi.org/10.1017/s0252921100092745.

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“Sonate” (Sondages acoustiques pour l’évaluation de la qualité d’images des téléscopes) – Acoustic sounding to estimate the quality of telescope images – is a prime example of professional/amateur collaboration as it involved 3 professionals and 22 amateurs, who, in order to collect the maximum amount of data, relayed one another in 10-day shifts over a period of 4 months in 1984, using the 1-m telescope at the Pic du Midi. A preliminary campaign with the 2-m telescope in 1982 had shown that the profile of sound waves reflected from the layers above a site could be correlated with the quality of telescopic images at the same site.

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20

Hasan, S. S. "The Indian National Large Solar Telescope (NLST)." Proceedings of the International Astronomical Union 5, S264 (August 2009): 499–504. http://dx.doi.org/10.1017/s1743921309993206.

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AbstractThe Indian National Large Solar Telescope (NLST) will be a state-of-the-art 2-m class telescope for carrying out high resolution studies of the solar atmosphere. Sites in the Himalayan region at altitudes greater than 4000-m that have extremely low water vapor content and are unaffected by monsoons are under evaluation. This project is led by the Indian Institute of Astrophysics and has national and international partners.NLST is an on-axis alt-azimuth Gregorian multi-purpose open telescope with the provision of carrying out night time stellar observations using a spectrograph. The telescope utilizes an innovative design with low number of reflections to achieve a high throughput and low instrumental polarization. High order adaptive optics is integrated into the design that works with a modest Fried's parameter of 7-cm to give diffraction limited performance. The telescope will be equipped with a suite of post-focus instruments including a high resolution spectrograph and a polarimeter. A detailed concept design of the telescope is presently being finalized and fabrication is expected to begin in 2010 with first light in 2014.

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21

Guélin, M., S. Garcia-Burillo, R. Blundell, J. Cernicharo, D. Despois, and H. Steppe. "The Molecular Spiral Structure in M51 Derived from CO(J=2-1) Line Observations." Highlights of Astronomy 8 (1989): 575–77. http://dx.doi.org/10.1017/s1539299600008406.

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22

Markarian, B. E., J. A. Stepanian, and L. K. Erastova. "The Second Byurakan Spectral Sky Survey." Symposium - International Astronomical Union 121 (1987): 25–35. http://dx.doi.org/10.1017/s0074180900154865.

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The method of the Second Spectral Survey carried out with the Byurakan 1-m Schmidt telescope is discussed. The limiting magnitude is fainter in comparison with the First Byurakan Survey at about 2–3m.The results of low dispersion (500 objects) and slit spectroscopy (300 objects) based on observations with the 6-m telescope of Special Astrophysical Observatory for four fields of the Second Survey are presented.The luminosity function of faint UV galaxies is discussed. The completeness of AGN of the Second Survey and their surface and space densities are also estimated. The surface density of QSO and ELG is estimated and these data are compared with the results of other surveys.New observational data obtained with the 6-m telescope are compared with the new data of different deep surveys carried out during last years.

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23

von der Lühe, O., W. Schmidt, D. Soltau, Th Berkefeld, F. Kneer, and J. Staude. "GREGOR: a 1.5 m telescope for solar research." Astronomische Nachrichten 322, no. 5-6 (December 2001): 353–60. http://dx.doi.org/10.1002/1521-3994(200112)322:5/6<353::aid-asna353>3.0.co;2-z.

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24

Eads, Ryker W., and J. Roger P. Angel. "A 20 m wide-field diffraction-limited telescope." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 379, no. 2188 (November 23, 2020): 20200141. http://dx.doi.org/10.1098/rsta.2020.0141.

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A 20 m space telescope is described with an unvignetted 1° field of view—a hundred times larger in area than fields of existing space telescopes. Its diffraction-limited images are a hundred times sharper than from wide-field ground-based telescopes and extend over much if not all the field, 40 arcmin diameter at 500 nm wavelength, for example. The optical system yielding a 1°, 1.36 m diameter image at f/3.9 has relatively small central obscuration, 9% by area on axis, and is fully baffled. Several carousel-mounted instruments can each access directly the full image. The initial instrument complement includes a 400 gigapixel silicon imager with 2 µm pixels (0.005 arcsec), and a 60 gigapixel HgCdTe imager with 5 µm pixels (0.012 arcsec). A multi-object spectrograph with 10 000 fibres will allow spectroscopy with 0.02 arcsec resolution. Direct imaging and spectroscopy of exoplanets can take advantage of the un-aberrated, on-axis image (5 nm RMS wavefront error). While this telescope could be built for operation in free space, a site accessible to a human outpost at the Moon's south pole would be advantageous, for assembly and repairs. The lunar site would allow also for the installation of new instruments to keep up with evolving scientific priorities and advancing technology. Cooling to less than 100E K would be achieved with a surrounding cylindrical thermal shield. This article is part of a discussion meeting issue ‘Astronomy from the Moon: the next decades’.

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25

Kawabata, Tetsuya, Kazuya Ayani, Mitsugu Fujii, Yuji Urata, Nobuyuki Kawai, and Noboru Ebizuka. "A Spectrograph for Prompt Observations of Gamma-Ray Bursts with a 1-m Telescope." International Astronomical Union Colloquium 183 (2001): 157–58. http://dx.doi.org/10.1017/s0252921100078787.

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AbstractWe are developing a new slit-less spectrograph for gamma-ray bursts (GRBs) at Bisei Astronomical Observatory. We can quickly point the 1-m telescope to the GRB coordinates provided by HETE-2 via the GRB Coordinates Network. The pointing is readjusted when the position is refined to 5” accuracy by the small optical telescope RIBOTS using the optical image of the GRB, and we then take an exposure immediately with the slit-less spectrograph.

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26

Ragazzoni, R., C. Arcidiacono, G. Bono, M. Busso, E. Diolaiti, J. Farinato, A. Moore, et al. "An adaptive 2 m class telescope for a microlensing search from Antarctica." EAS Publications Series 14 (2005): 161–67. http://dx.doi.org/10.1051/eas:2005025.

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27

Zhao, Y., J. Zhong, J. Wei, J. Hu, and Q. Li. "Optical Identification of the ROSAT All-Sky Survey Sources in Two 2° × 2° Fields." International Astronomical Union Colloquium 159 (1997): 427–28. http://dx.doi.org/10.1017/s0252921100040653.

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AbstractWe used the CCD camera and spectrograph of the 2.16-m telescope of Beijing Astronomical Observatory to identify the ROSAT All-Sky survey sources in two 2° Ü 2° fields. Of a total of 16 X-ray sources, we identified 13 of them as follows: two QSOs, two Seyfert galaxies, two active galaxies, two clusters of galaxies, and five late-type stars. Three X-ray sources remained unidentified.

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28

Livingston, W. "A 4-meter McMath Telescope for the Infrared." Symposium - International Astronomical Union 154 (1994): 589–94. http://dx.doi.org/10.1017/s007418090012488x.

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Having no window and a filled aperture, i.e., no occlusion by secondary optics, the all-reflective McMath telescope is a proven IR facility. Beyond about 2 μm, it is diffraction limited, however. Engineering studies show that the McMath building could accommodate an increase to a 4-m aperture with a 6-m alt-azimuth feed, permitting sub-arcsec resolution to 12 μm. The use of cooled, solid aluminum mirrors would eliminate “mirror seeing”, which plagues non-vacuum solar telescopes.

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29

Tercero, F., J. A. López-Pérez, J. D. Gallego, F. Beltrán, O. García, M. Patino-Esteban, I. López-Fernández, et al. "Yebes 40 m radio telescope and the broad band Nanocosmos receivers at 7 mm and 3 mm for line surveys." Astronomy & Astrophysics 645 (January 2021): A37. http://dx.doi.org/10.1051/0004-6361/202038701.

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Context. Yebes 40 m radio telescope is the main and largest observing instrument at Yebes Observatory and is devoted to very long baseline interferometry (VLBI) and single-dish observations since 2010. It has been covering frequency bands between 2 GHz and 90 GHz in discontinuous and narrow windows in most cases in order to match the current needs of the European VLBI Network (EVN) and the Global Millimeter VLBI Array (GMVA). Aims. The Nanocosmos project, a European Union-funded synergy grant, has enabled an increase in the instantaneous frequency coverage of the Yebes 40 m radio telescope, making it possible to observe many molecular transitions with single tunings in single-dish mode. This reduces the observing time and maximises the output from the telescope. Methods. We present technical specifications of the recently installed 31.5−50 GHz (Q band) and 72−90.5 GHz (W band) receivers along with the main characteristics of the telescope at these frequency ranges. We observed IRC+10216, CRL 2688, and CRL 618, which harbour a rich molecular chemistry, to demonstrate the capabilities of the new instrumentation for spectral observations in single-dish mode. Results. Our results show the high sensitivity of the telescope in the Q band. The spectrum of IRC+10126 offers an unprecedented signal-to-noise ratio for this source in this band. On the other hand, the spectrum normalised by the continuum flux towards CRL 618 in the W band demonstrates that the 40 m radio telescope produces comparable results to those from the IRAM 30 m radio telescope, although with a lower sensitivity. The new receivers fulfil one of the main goals of Nanocosmos and open up the possibility to study the spectrum of different astrophysical media with unprecedented sensitivity.

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30

Aizu, Ko, Makoto Inoue, Hiroto Tabara, and Tatsnji Kato. "Search for Extragalactic Radio Sources with Large Rotation Measure." Symposium - International Astronomical Union 140 (1990): 472. http://dx.doi.org/10.1017/s0074180900190904.

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Intrinsic large rotation measures (RM) were searched for 128 extragalactic sources based on polarization data obtained at the NRO 45–m telescope. The number of sources with RM > 500 rad m−2 is only seven.

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31

Mould, Jeremy. "A Next Generation Deep 2-μm Survey: Reconnoitering the Dark Ages." Publications of the Astronomical Society of Australia 28, no. 3 (2011): 266–70. http://dx.doi.org/10.1071/as11036.

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AbstractThe next generation 2-μm sky survey should target nascent galaxies in the epoch of reionization for spectroscopic followup on large telescopes. A 2.5-m telescope at a site on the Antarctic plateau has advantages for this purpose and for southern hemisphere infrared surveys in general.

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32

Bochkarev, N. G. "Russian/Former Soviet Union Experience in Professional Small Telescope Usage." International Astronomical Union Colloquium 183 (2001): 345–51. http://dx.doi.org/10.1017/s0252921100079276.

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FSU astronomers traditionally use small telescopes (⊘ ≤1.5 m, hereafter STs) for both science and education. Russian/FSU experience here is among the largest world-wide. There are only 2 large and moderate-sized facilities in whole Russia: the 6 m telescope of SAO RAS and Russian-Ukrainian 2 m one on the 3100 m high peak Terskol in Central Caucasus.Equipped with good light receivers and handled by skilled observers, STs can produce first class scientific data. Important results are typically yielded by long-time sequences of observations and/or new observational “know how”: good instrument/receiver design, appropriate selection of objects and moments, etc. Examples of what has been done with STs in FSU, within my memory, (in the last ≃ 1/3 century) are listed below, without a list of references, because of lack of space. The author plans to publish a larger article on this subject in Astr.&Aph.Trans.

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33

Cho, Se-Hyung. "Observations of SiO J=2–1 and J=3–2 masers towards evolved stars with the TRAO 14 m telescope." Proceedings of the International Astronomical Union 3, S242 (March 2007): 314–15. http://dx.doi.org/10.1017/s1743921307013191.

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AbstractWe present the results of survey and time-monitoring observations of SiO J=2–1 and J=3–2 masers towards evolved stars with the 14 m radio telescope at Taeduk Radio Astronomy Observatory (TRAO) from 1995 February to 2001 February. The first detection of SiO v=3, J=2–1 maser emission toward S-type Mira variable χ Cyg is also presented.

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34

Saleck, A. H., R. Simon, G. Winnewisser, and J. G. A. Wouterloot. "Detection of interstellar 13CCH and C13CH." Canadian Journal of Physics 72, no. 11-12 (November 1, 1994): 747–54. http://dx.doi.org/10.1139/p94-098.

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We report an unambiguous detection of the 13CCH and C13CH isotopomers of the ethynyl radical towards the Orion A ridge by identification of their N = 2 → 1 transitions. The observations have been made with the IRAM 30 m telescope at Pico Veleta, Spain. By these measurements, we confirm an earlier tentative detection of four hyperfine components of C13CH with the KOSMA 3 m telescope at Gornergrat, Switzerland. Although uncertainties in the calibration of line intensities are not completely settled, these observations suggest that C13CH might be the more abundant of the two 13C isotopomers. This tentative finding pertains towards the region where the emission of molecular radicals peaks, i.e., northeast of the Kleinmann–Low nebula. Furthermore, the N = 1 → 0 transition of C13CH has been detected in the same region with the SEST 15 m telescope at La Silla, Chile. In combination with the laboratory N = 4 ← 3 and N = 5 ← 4 data, we derive improved ground state rotational constants for both species.

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35

Dekany, Richard, Jennifer Roberts, Rick Burruss, Antonin Bouchez, Tuan Truong, Christoph Baranec, Stephen Guiwits, et al. "PALM-3000: EXOPLANET ADAPTIVE OPTICS FOR THE 5 m HALE TELESCOPE." Astrophysical Journal 776, no. 2 (October 7, 2013): 130. http://dx.doi.org/10.1088/0004-637x/776/2/130.

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36

Malpas, Amber, Michael D. Albrow, Jennifer C. Yee, Andrew Gould, Andrzej Udalski, Antonio Herrera Martin, Charles A. Beichman, et al. "OGLE-2017-BLG-1038: A Possible Brown-dwarf Binary Revealed by Spitzer Microlensing Parallax." Astronomical Journal 164, no. 3 (August 18, 2022): 102. http://dx.doi.org/10.3847/1538-3881/ac7d4c.

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Abstract We report the analysis of microlensing event OGLE-2017-BLG-1038, observed by the Optical Gravitational Lensing Experiment, Korean Microlensing Telescope Network, and Spitzer telescopes. The event is caused by a giant source star in the Galactic Bulge passing over a large resonant binary-lens caustic. The availability of space-based data allows the full set of physical parameters to be calculated. However, there exists an eightfold degeneracy in the parallax measurement. The four best solutions correspond to very-low-mass binaries near ( M 1 = 170 − 50 + 40 M J and M 2 = 110 − 30 + 20 M J ), or well below ( M 1 = 22.5 − 0.4 + 0.7 M J and M 2 = 13.3 − 0.3 + 0.4 M J ) the boundary between stars and brown dwarfs. A conventional analysis, with scaled uncertainties for Spitzer data, implies a very-low-mass brown-dwarf binary lens at a distance of 2 kpc. Compensating for systematic Spitzer errors using a Gaussian process model suggests that a higher mass M-dwarf binary at 6 kpc is equally likely. A Bayesian comparison based on a galactic model favors the larger-mass solutions. We demonstrate how this degeneracy can be resolved within the next 10 years through infrared adaptive-optics imaging with a 40 m class telescope.

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Casamiquela, Laia, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, and Caroline Soubiran. "Chemically Peculiar Stars in the Open Cluster Stock 2." Astronomical Journal 164, no. 6 (November 18, 2022): 255. http://dx.doi.org/10.3847/1538-3881/ac9c56.

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Abstract The recently rediscovered open cluster Stock 2, located roughly 375 pc away and about 400 Myr old, has the potential to be an exciting new testbed for our understanding of stellar evolution. We present results from a spectroscopic campaign to characterize stars near the cluster’s main-sequence turnoff; our goal is to identify candidate chemically peculiar stars among the cluster’s A stars. We obtained échelle spectra for 64 cluster members with ESPaDOnS on the 3.6 m Canada–France–Hawaii Telescope, Maunakea Observatory, USA, and for six stars with SOPHIE on the 1.93 m telescope at the Observatoire de Haute-Provence, France. We complemented these new observations with those of 13 high-mass cluster members from the HARPS-N archive; our overall sample is of 71 stars. We derived the fundamental parameters (T eff, log g , [M/H]) as well as v e sin i for our sample using the sliced inverse regression technique, and then used iSpec to derive individual abundances of 12 chemical species. With these abundance determinations, we identified nine A stars with anomalous levels of Sc, Ca, and other metallic lines. Follow-up observations of these Am candidates with a known age can transform them into benchmarks for evolutionary models that include atomic diffusion and help build a better understanding of the complex interactions between macroscopic and microscopic processes in stellar interiors.

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Chen, J. L., J. S. Zhang, C. Henkel, Y. T. Yan, H. Z. Yu, J. J. Qiu, X. D. Tang, et al. "Interstellar Nitrogen Isotope Ratios: New NH₃ Data from the Galactic Center out to the Perseus Arm." Astrophysical Journal Supplement Series 257, no. 2 (November 24, 2021): 39. http://dx.doi.org/10.3847/1538-4365/ac205a.

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Abstract Our aim is to measure the interstellar 14N/15N ratio across the Galaxy, to establish a standard data set on interstellar ammonia isotope ratios, and to provide new constraints on the Galactic chemical evolution. The (J, K) = (1, 1), (2, 2), and (3, 3) lines of 14NH3 and 15NH3 were observed with the Shanghai Tianma 65 m radio telescope (TMRT) and the Effelsberg 100 m telescope toward a large sample of 210 sources. One hundred fourty-one of these sources were detected by the TMRT in 14NH3. Eight of them were also detected in 15NH3. For 10 of the 36 sources with strong NH3 emission, the Effelsberg 100 m telescope successfully detected their 15NH3(1, 1) lines, including 3 sources (G081.7522, W51D, and Orion-KL) with detections by the TMRT telescope. Thus, a total of 15 sources are detected in both the 14NH3 and 15NH3 lines. Line and physical parameters for these 15 sources are derived, including optical depths, rotation and kinetic temperatures, and total column densities. 14N/15N isotope ratios were determined from the 14NH3/15NH3 abundance ratios. The isotope ratios obtained from both telescopes agree for a given source within the uncertainties, and no dependence on heliocentric distance and kinetic temperature is seen. 14N/15N ratios tend to increase with galactocentric distance, confirming a radial nitrogen isotope gradient. This is consistent with results from recent Galactic chemical model calculations, including the impact of superasymptotic giant branch stars and novae.

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Currie, Miles H., Victoria S. Meadows, and Kaitlin C. Rasmussen. "There’s More to Life than O₂: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets." Planetary Science Journal 4, no. 5 (May 1, 2023): 83. http://dx.doi.org/10.3847/psj/accf86.

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Abstract Within the next decade, atmospheric O2 on Earth-like M-dwarf planets may be accessible with visible–near-infrared (NIR), high-spectral-resolution, ground-based extremely large telescope (ELT) instruments. However, the prospects for using ELTs to detect environmental properties that provide context for O2 have not been thoroughly explored. Additional molecules may help indicate planetary habitability, rule out abiotically generated O2, or reveal alternative biosignatures. To understand the accessibility of environmental context using ELT spectra, we simulate high-resolution transit transmission spectra of previously generated evolved terrestrial atmospheres. We consider inhabited preindustrial and Archean Earth–like atmospheres, and lifeless worlds with abiotic O2 buildup from CO2 and H2O photolysis. All atmospheres are self-consistent with M2V–M8V dwarf host stars. Our simulations include explicit treatment of systematic and telluric effects to model high-resolution spectra for Giant Magellan Telescope (GMT), Thirty Meter Telescope (TMT), and European ELT (E-ELT) configurations for systems 5 and 12 pc from Earth. Using the cross-correlation technique, we determine the detectability of major species in these atmospheres: O2, O3, CH4, CO2, CO, H2O, and C2H6. Our results suggest that CH4 and CO2 are the most accessible molecules for terrestrial planets transiting a range of M-dwarf hosts using an E-ELT-, TMT-, or GMT-sized telescope, and that the O2 NIR and H2O 0.9 μm bands may also be accessible with more observation time. Although this technique still faces considerable challenges, the ELTs will provide access to the atmospheres of terrestrial planets transiting earlier-type M-dwarf hosts that may not be possible using JWST.

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Kuno, N., T. Tosaki, S. Onodera, R. Miura, K. Muraoka, S. Komugi, T. Sawada, et al. "NRO Legacy Project: M33 all Disk Survey of Giant Molecular Clouds with NRO 45-m and ASTE 10-m telescopes." Proceedings of the International Astronomical Union 6, S277 (December 2010): 67–70. http://dx.doi.org/10.1017/s1743921311022484.

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AbstractWe have conducted all disk imaging of M33 in 12CO(1-0) using the 45-m telescope at Nobeyama Radio Observatory. We present preliminary results of this project. The spatial resolution of ~ 80 pc is comparable to the size of GMCs. The identified GMCs show wide variety in star forming activity. The variety can be regarded as the difference of their evolutionary stage. We found that Kennicutt-Schmidt law breaks in GMC scale (~ 80 pc), although it is still valid in 1 kpc scale. The correlation between molecular gas fraction, fmol = Σ(H2)/Σ(HI+H2) and gas surface density shows two distinct sequences and shows that fmol tends to be higher near the center. We also made partial mapping 12CO(3-2) with ASTE telescope. These data show that the variation of physical properties of molecular gas are correlated with the GMC evolution and mass. That is, GMCs with more active star formation and more mass tend to have higher fraction of dense gas.

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Jia, Peng, and SiJiong Zhang. "Performance modeling of the adaptive optics system on the 2.16 m telescope." Science China Physics, Mechanics and Astronomy 56, no. 3 (February 13, 2013): 658–62. http://dx.doi.org/10.1007/s11433-013-5028-2.

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42

Gao Zechao, 高则超, 郝. 亮. Hao Liang, 王富国 Wang Fuguo, 张丽敏 Zhang Limin, 王. 瑞. Wang Rui, and 范. 磊. Fan Lei. "Design and optimization of active adjusting lateral support mechanism for 2 m telescope." Infrared and Laser Engineering 48, no. 8 (2019): 814001. http://dx.doi.org/10.3788/irla201948.0814001.

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43

Burton, M. G. "The Science Case for a 2 m-class Telescope at Dome C, Antarctica." EAS Publications Series 25 (2007): 103–10. http://dx.doi.org/10.1051/eas:2007080.

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Kameya, Osamu, Tatsuhiko Hasegawa, Naomi Hirano, Keiya Takakubo, and Munezo Seki. "CS(J = 2-1) Observations of B335." Symposium - International Astronomical Union 115 (1987): 366–67. http://dx.doi.org/10.1017/s0074180900095899.

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CS(J = 2-1) observations of B335 are carried out using the NRO 45-m telescope with a 16″ beam. We get many self-reversed profiles with good S/N ratio. Assuming that this region consists of a core and a halo, we get the molecular hydrogen density and the CS relative abundance in the halo. The CS wings are located within the cavity of the CO wing (Goldsmith et al. 1984).

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Cotton, Daniel V., Jeremy Bailey, Jeff Larson, Wm Bruce Weaver, Jean Perkins, and Glenn Henderson. "HIPPI-2 Commissioned at MIRA." Research Notes of the AAS 6, no. 10 (October 14, 2022): 209. http://dx.doi.org/10.3847/2515-5172/ac996d.

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Abstract We have commissioned the High Precision Polarimetric Instrument 2 on the Monterey Institute for Research in Astronomy's 36 inch telescope at its Bernard M. Oliver Observing Station. The night-to-night precision on bright stars is measured as σ p = 7.1 ppm and e p = 1.7 ppm in g ′ ; its accuracy on high polarization standard stars is 1.2%, despite the instrument not being actively guided. This matches the best performance achieved on much larger telescopes, which we attribute to the excellent site conditions.

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Li, Jie, Fengtao Yan, Lin Chen, Jie Yang, and Yongjian Wan. "Measurement Vertex Position of a Large Aspheric Mirror." Applied Sciences 9, no. 6 (March 13, 2019): 1038. http://dx.doi.org/10.3390/app9061038.

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We present a novel method to accurately measure the vertex position of a large aspheric mirror with a phasing measuring interferometer, a laser tracker, and a micro alignment telescope. The method consists of rotating the mirror by 180° about its mechanical axis and measuring the change in displacement. Use of a micro alignment telescope eliminates the need to adjust the mirror during the measurement, eases the alignment of the testing system, and improves the vertex position measurement accuracy. Using this method, we measured the vertex position of an aspheric mirror 1 m in diameter and 2 m in radius of curvature. The vertex position measurement uncertainty is 88 μm.

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47

Muraoka, K., K. Kohno, T. Tosaki, N. Kuno, K. Nakanishi, K. Sorai, and S. Sakamoto. "ASTE CO(3-2) observations of M 83: Correlation between CO(3-2)/CO(1-0) ratios and star formation efficiencies." Proceedings of the International Astronomical Union 2, S237 (August 2006): 451. http://dx.doi.org/10.1017/s1743921307002396.

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AbstractWe have performed CO(J=3−2) emission observations with the Atacama Submillimeter Telescope Experiment (ASTE) toward the 5′ × 5′ (or 6.6 × 6.6 kpc at the distance D = 4.5 Mpc) region of the nearby barred spiral galaxy M 83. We successfully resolved the major structures, i.e., the nuclear starburst region, bar, and inner spiral arms in CO(J=3−2) emission at a resolution of 22'' (or 480 pc), showing a good spatial coincidence between CO(J=3−2) and 6 cm continuum emissions.From a comparison of CO(J=3−2) data with CO(J=1−0) intensities measured with Nobeyama 45-m telescope, we found that the radial profile of CO(J=3−2)/CO(J=1−0) integrated intensity ratio R3−2/1−0 is almost unity in the central region (r<0.25 kpc), whereas it drops to a constant value, 0.6–0.7, in the disk region. The radial profile of star formation efficiencies (SFEs), determined from 6 cm radio continuum and CO(J=1−0) emission, shows the same trend as that of R3−2/1−0. At the bar-end (r ~ 2.4 kpc), the amounts of molecular gas and the massive stars are enhanced when compared with other disk regions, whereas there is no excess of R3−2/1−0 and SFE in that region. This means that a simple summation of the star forming regions at the bar-end and the disk cannot reproduce the nuclear starburst of M 83, implying that the spatial variation of the dense gas fraction traced by R3−2/1−0 governs the spatial variation of SFE in M 83.

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Richards, Joseph L., Walter Max-Moerbeck, Vasiliki Pavlidou, Oliver G. King, Timothy J. Pearson, Anthony C. S. Readhead, Rodrigo Reeves, et al. "BLAZARS IN THE FERMI ERA: THE OVRO 40 m TELESCOPE MONITORING PROGRAM." Astrophysical Journal Supplement Series 194, no. 2 (May 23, 2011): 29. http://dx.doi.org/10.1088/0067-0049/194/2/29.

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49

Burton, M. G., J. S. Lawrence, M. C. B. Ashley, J. A. Bailey, C. Blake, T. R. Bedding, J. Bland-Hawthorn, et al. "Science Programs for a 2-m Class Telescope at Dome C, Antarctica: PILOT, the Pathfinder for an International Large Optical Telescope." Publications of the Astronomical Society of Australia 22, no. 3 (2005): 199–235. http://dx.doi.org/10.1071/as04077.

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AbstractThe cold, dry, and stable air above the summits of the Antarctic plateau provides the best ground-based observing conditions from optical to sub-millimetre wavelengths to be found on the Earth. Pathfinder for an International Large Optical Telescope (PILOT) is a proposed 2 m telescope, to be built at Dome C in Antarctica, able to exploit these conditions for conducting astronomy at optical and infrared wavelengths. While PILOT is intended as a pathfinder towards the construction of future grand-design facilities, it will also be able to undertake a range of fundamental science investigations in its own right. This paper provides the performance specifications for PILOT, including its instrumentation. It then describes the kinds of projects that it could best conduct. These range from planetary science to the search for other solar systems, from star formation within the Galaxy to the star formation history of the Universe, and from gravitational lensing caused by exo-planets to that produced by the cosmic web of dark matter. PILOT would be particularly powerful for wide-field imaging at infrared wavelengths, achieving near diffraction-limited performance with simple tip–tilt wavefront correction. PILOT would also be capable of near diffraction-limited performance in the optical wavebands, as well be able to open new wavebands for regular ground-based observation, in the mid-IR from 17 to 40 μm and in the sub-millimetre at 200 μm.

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Stockman, H. S., and John C. Mather. "The Next Generation Space Telescope." Symposium - International Astronomical Union 204 (2001): 467–74. http://dx.doi.org/10.1017/s0074180900226429.

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The Next Generation Space Telescope (NGST) will be an 8 m deployable telescope, radiatively cooled to 30 K and diffraction-limited at 2 μm, operating at the Sun-Earth Lagrangian point L2. It will be built by a partnership of NASA, ESA, and CSA (Canadian Space Agency). The camera sensitivity should be limited by the zodiacal light for wavelengths < 10 μm. The main scientific objectives are the study of the origin and evolution of galaxies, stars, and planets, beginning with the first luminous objects to form from the Big Bang. Other objectives include studies of dark matter, supernovae, the intergalactic medium, gamma ray bursts, star ages, and exobiology. The telescope will be operated like the Hubble Space Telescope (HST) by the Space Telescope Science Institute, with all observing programs openly solicited and selected by peer review.The NGST scientific requirements originated with the report of the Dressler Committee HST & Beyond. The instruments recommended by the Ad Hoc Science Working Group (ASWG) include 1) a wide field near infrared (NIR) camera with an 8K2 detector array covering 0.6 - 5 μm, 2) a multi-object NIR spectrograph capable of simultaneously observing > 100 objects with a resolution of R (λ/δλ) = 1000, and 3) a combined mid-infrared (MIR) camera and spectrograph from 5-27 μm, with a resolution of R > 1500.

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