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Relevant bibliographies by topics / Near IR high resolution astronomical spectrograph

Academic literature on the topic 'Near IR high resolution astronomical spectrograph'

Author: Grafiati

Published: 10 March 2023

Last updated: 11 March 2023

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Journal articles on the topic "Near IR high resolution astronomical spectrograph"

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Bundy, Kevin, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, et al. "The Stability of Fiber Spectrographs in the Faint-source Regime." Astronomical Journal 164, no. 3 (August 11, 2022): 94. http://dx.doi.org/10.3847/1538-3881/ac76cc.

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Abstract The use of optical fibers in astronomical instrumentation offers high-multiplex and light-gathering flexibility. However, with most previous fiber spectrographs optimized for large fields of view on modest-aperture telescopes, the performance of fibers in the context of faint targets on large telescopes remains largely untested. In this paper, we evaluate aspects of fiber stability, especially as they apply in the context of precision sky subtraction of faint sources at modest spectral resolution (R ∼ 3000). After introducing a framework for describing potential systematic errors, we use publicly available data from existing instruments, including instrumentation used by the fourth-generation Sloan Digital Sky Survey’s MaNGA project (MaNGA: Mapping Nearby Galaxies at Apache Point Observatory) and the Very Large Telescope’s FLAMES: Fiber Large Array Multi Element Spectrograph. We isolate sources of fiber systematics and estimate the observed amplitude of persistent residuals as well as stochastic noise contributions resulting from changing fiber stresses. Comparing these levels against their impact on various sky subtraction schemes demonstrates that 0.1% precision sky subtraction with fiber instruments is possible. As a demonstration, we show that the MaNGA instrument can deliver 0.2% residuals on bright near-IR sky lines with nonlocal sky subtraction, if pseudo-slit limitations are addressed by allocating 50% of its fibers to sky. We further highlight recently published deep exposures that achieved a 1σ background level of 27.6 AB per square arc second, equivalent to a precision of 0.2% of the sky background continuum.

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Iliev, Lubomir. "Recent Spectral Observations of Epsilon Aurigae in the Near-IR." Proceedings of the International Astronomical Union 7, S282 (July 2011): 95–96. http://dx.doi.org/10.1017/s1743921311027062.

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AbstractHigh resolution spectral observations of ϵ Aur were carried out in the near-IR spectral range. Observations were obtained with the Coudé-spectrograph of the 2m RCC telescope at National Astronomical Observatory Rozhen and cover all main phases of the current eclipse. Results revealed for the first time absorption components in O I and Ca II triplets and variations of N I lines. Estimation of the electron density was done using lines from the Paschen series of hydrogen.

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Origlia, L., and E. Oliva. "SIMPLE: A High Resolution Near IR Spectrograph for the European ELT." Earth, Moon, and Planets 105, no. 2-4 (July 8, 2009): 123–26. http://dx.doi.org/10.1007/s11038-009-9335-6.

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Ikeda, Yuji, Sohei Kondo, Shogo Otsubo, Satoshi Hamano, Chikako Yasui, Noriyuki Matsunaga, Hiroaki Sameshima, et al. "Highly Sensitive, Non-cryogenic NIR High-resolution Spectrograph, WINERED." Publications of the Astronomical Society of the Pacific 134, no. 1031 (January 1, 2022): 015004. http://dx.doi.org/10.1088/1538-3873/ac1c5f.

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Abstract WINERED is a novel near-infrared (NIR) high-resolution spectrograph (HRS) that pursues the highest possible sensitivity to realize high-precision spectroscopy in the NIR as in the optical wavelength range. WINERED covers 0.9–1.35 μm (z, Y, and J-bands) with three modes (Wide mode and two Hires modes) at the maximum spectral resolutions of R = 28,000 and R = 70,000. For fulfilling the objective, WINERED is designed with an unprecedentedly high instrument throughput (up to 50% at maximum including the quantum efficiency of the array) that is three times or more than other existing optical/NIR HRSs. This is mainly realized by a combination of non-white pupil and no fiber-fed configuration in optical design, the moderate (optimized) wavelength coverage, and the high-throughput gratings. Another prominent feature of WINERED is “warm” instrument despite for infrared (IR) observations. Such non-cryogenic (no cold stop) IR instrument finally became possible with the combination of custom-made thermal-cut filter of 10−8 class, 1.7 μm cutoff HAWAII-2RG array, and a cold baffle reducing the direct thermal radiation to the IR array into the solid angle of f/2. The thermal background is suppressed below 0.1 photons pixel−1 s−1 even in the wide band of 0.9–1.35 μm under the environment of 290 K. WINERED had been installed to the 3.58 m New Technology Telescope at La Silla Observatory, ESO, since 2017. Even with the intermediate size telescope, WINERED was confirmed to provide a limiting magnitude (for SNR = 30 with 8 hr. integration time) of J = 16.4 mag for the Wide mode and J = 15.1 mag for the Hires mode, respectively, under the natural seeing conditions. These sensitivities are comparable to those for the existing NIR-HRSs attached to the 8–10 m class telescopes with AO. WINERED type spectrographs may become a critical not only for the currently on-going extremely large telescopes to reduce the developing cost and time but also for smaller telescopes to extend their lives with long programs.

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McGregor, Peter J., Peter Conroy, Gabe Bloxham, and Jan van Harmelen. "Near-infrared Integral-Field Spectrograph (NIFS): An Instrument Proposed for Gemini." Publications of the Astronomical Society of Australia 16, no. 3 (1999): 273–87. http://dx.doi.org/10.1071/as99273.

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AbstractIn late 1998 the International Gemini Project Office identified a need for a low cost, near-infrared spectrograph to be commissioned on the Gemini South telescope on the shortest possible timescale. In response, the Research School of Astronomy and Astrophysics of the Australian National University proposed to design, construct, and commission a near-infrared, integral-field spectrograph on Gemini. The science drivers and novel design of the Near-infrared Integral-Field Spectrograph (NIFS) are described in this paper. NIFS will achieve significant economies in cost and schedule in several ways:• By addressing targeted science with high efficiency. NIFS will primarily target velocity measurements in galaxies to study the demographics of black holes in galactic nuclei and the evolution of structural properties in high redshift galaxies. However, NIFS will also be applied to a wide range of general astronomical topics, but these will not dictate the instrument design.• By adopting a largely fixed-format design. A 3·2″ × 3·2″ ‘stair-case’ integral field unit (IFU) will feed a near-infrared spectrograph with four fixed-angle gratings mounted on a single grating wheel. A single, fixed-format camera will form the spectral image on a 2048 × 2048 Rockwell HgCdTe HAWAII-2 array. Two-pixel spectral resolving powers of ∼5400 will be achieved with complete wavelength coverage in each of the J, H, and K photometric bands through 32 optimally sampled 0·1″ wide slitlets. The velocity resolution of ∼55 km s−1 will be sufficient to achieve the targeted science objectives, and will allow software rejection of OH airglow lines.• By packaging the NIFS instrument within a duplicate of the Near-Infrared Imager (NIRI) cryostat. The NIRI cryostat, On-Instrument Wavefront Sensor (OIWFS), detector focusing mechanism, control system, and EPICS software will all be duplicated with only minimal change. Construction of the duplicate NIRI cryostat, OIWFS, and control system will be done by the University of Hawaii.

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Ueta, Toshiya, David Fong, and Margaret Meixner. "Westbrook's Molecular Gun: Discovery of Near-Infrared Microstructures and Molecular Bullets in AFGL 618." Symposium - International Astronomical Union 209 (2003): 122. http://dx.doi.org/10.1017/s0074180900208279.

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We present high-sensitivity near-IR images of a carbon-rich proto-planetary nebula, AFGL 618, obtained with the Infrared Camera and Spectrograph (IRCS) mounted on the 8.2m Subaru Telescope. The deep near-IR images have revealed “bullets” and “horns” extending farther out from the edges of the previously known bipolar nebulosities that consist of dust-scattered star light component and shock-excited line emission component. That these bullets and horns represent the positions from which [Fe II] IR lines arise is strongly suggested from the spatial coincidence between these near-IR microstructures and the optical collimated outflow structure observed by the recent HST/WFPC2 imaging, together with the previous detection of shock-excited, forbidden IR lines of atomic species at those locations. At these positions of the near-IR mincrostructures, we have also discovered CO clumps moving at > 200 km s-1 from our re-analysis of the existing 12CO J = 1 – 0 data obtained with the Berkeley-Illinois-Maryland Association (BIMA) interferometer array. These findings indicate that fast-moving CO clumps seem to be impinging upon the surrounding ambient circumstellar shell, thereby causing shocked emission regions which manifest themselves as the near-IR microstructures at the shock interface. To deepen our understanding of the connection between the near-IR microstructures and the CO outflow structure, we are currently conducting higher resolution observation in CO lines with the BIMA array.

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Oliva, E., M. Rainer, A. Tozzi, N. Sanna, M. Iuzzolino, and A. Brucalassi. "Experimental characterization of modal noise in multimode fibers for astronomical spectrometers." Astronomy & Astrophysics 632 (November 21, 2019): A21. http://dx.doi.org/10.1051/0004-6361/201936610.

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Context. High resolution spectroscopy at high signal-to-noise ratios (S/Ns) is one the key techniques of the quantitative study of the atmospheres of extrasolar planets. Observations at near-infrared wavelengths with fiber-fed spectrographs coupled to extremely large telescopes are particularly important to tackle the ultimate goal of detecting biosignatures in rocky planets. Aims. To achieve high S/Ns in fiber-fed spectrogrpahs, the systematic noise effects introduced by the fibers must be properly understood and mitigated. In this paper we concentrate on the effects of modal noise in multimode fibers. Methods. Starting from our puzzling on-sky experience with the GIANO-TNG spectrometer we set up an infrared high resolution spectrometer in our laboratory and used this instrument to characterize the modal noise generated in fibers of different types (circular and octagonal) and sizes. Our experiment includes two conventional scrambling systems for fibers: a mechanical agitator and an optical double scrambler. Results. We find that the strength of the modal noise primarily depends on how the fiber is illuminated. It dramatically increases when the fiber is under-illuminated, either in the near field or in the far field. The modal noise is similar in circular and octagonal fibers. The Fourier spectrum of the noise decreases exponentially with frequency; i.e., the modal noise is not white but favors broad spectral features. Using the optical double scrambler has no effect on modal noise. The mechanical agitator has effects that vary between different types of fibers and input illuminations. In some cases this agitator has virtually no effect. In other cases, it mitigates the modal noise, but flattens the noise spectrum in Fourier space; i.e., the mechanical agitator preferentially filters the broad spectral features. Conclusions. Our results show that modal noise is frustratingly insensitive to the use of octagonal fibers and optical double scramblers; i.e., the conventional systems used to improve the performances of spectrographs fed via unevenly illuminated fibers. Fiber agitation may help in some cases, but its effect has to be verified on a case-by-case basis. More generally, our results indicate that the design of the fiber link feeding a spectrograph should be coupled with laboratory measurements that reproduce, as closely as possible, the conditions expected at the telescope.

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Siebenmorgen, R., P. Scicluna, and J. Krełowski. "Far-infrared emission of massive stars." Astronomy & Astrophysics 620 (November 23, 2018): A32. http://dx.doi.org/10.1051/0004-6361/201833546.

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We present results of the analysis of a sample of 22 stars of spectral types from O7 to B5 and luminosity classes I–V for which spectra from the Infrared Spectrograph (IRS) of Spitzer are available. The IRS spectra of these stars are examined for signs of excess infrared (IR) emission by comparison with stellar atmospheric spectra. We find that the spectra of half of the studied stars are dominated by excess emission in the far-IR, including all six super- and bright giants. In order to examine the origin of the far-IR excess, we supplement the Spitzer data with optical high-resolution echelle spectroscopy (λ∕Δλ ~ 105), near-IR high-contrast coronagraphic imaging taken with the SPHERE instrument at VLT with a spatial resolution of 0.′′05, and WISE and Herschel photometry. In the optical region, we detect various absorption and emission lines (H α, C III, and N III) irrespective of the far-IR excess. Pfund α and Humphrey α lines are observed at the same time as the far-IR excess. These lines are stronger in stars with far-IR excess than in stars without excess. A scattered-light disk in the central r ≲ 2.5′′ region of the far-IR excess stars HD 149404, HD 151804, and HD 154368 can be excluded from H band imaging down to a 1σ contrast of F(r)∕F∗~ 10−6. The far-IR excess is fit either by a free–free component from ionized gas as for the winds of hot stars or a large (1 pc) circumstellar dust shell. The putative dust envelopes required to explain the excess have a visual extinction as low as a few hundred μ-mag.

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Sarre, P. J., and T. R. Kendall. "Diffuse Interstellar Bands." Symposium - International Astronomical Union 197 (2000): 343–48. http://dx.doi.org/10.1017/s0074180900164927.

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The unidentified diffuse interstellar bands are observed in near-UV, visible and near-IR spectra recorded towards stars which are partially obscured by interstellar dust. Their origin is the longest standing problem in astronomical spectroscopy and dates back to the 1930s when systematic study of the bands first started. Proposals for the carriers range from molecular hydrogen to porphyrins and from colour centres to species adsorbed on grain surfaces. This paper contains a short review of the problem and a discussion of recent possible assignments of some of the bands to transitions of the H2, and molecules. Observations of ultra-high resolution spectra of diffuse absorption bands, optical diffuse emission bands from the Red Rectangle, and complementary studies of the 3.3 μm ‘unidentified’ infrared (UIR) emission band are described.

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Hamano, Satoshi, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, et al. "Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands." Astrophysical Journal Supplement Series 262, no. 1 (August 17, 2022): 2. http://dx.doi.org/10.3847/1538-4365/ac7567.

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Abstract We searched for diffuse interstellar bands (DIBs) in the 0.91 < λ < 1.33 μm region by analyzing the near-infrared (NIR) high-resolution (R = 20,000 and 28,000) spectra of 31 reddened early-type stars (0.04 < E(B − V) < 4.58) and an unreddened reference star. The spectra were collected using the WINERED spectrograph, which was mounted on the 1.3 m Araki telescope at Koyama Astronomical Observatory, Japan, in 2012–2016, and on the 3.58 m New Technology Telescope at La Silla Observatory, Chile, in 2017–2018. We detected 54 DIBs—25 of which are newly detected by this study—and eight DIB candidates. Using this updated list, the DIB distributions over a wide wavelength range, from optical to NIR, are investigated. The FWHM values of the NIR DIBs are found to be narrower than those of the optical DIBs, on average, which suggests that the DIBs at longer wavelengths tend to be caused by larger molecules. Assuming that the larger carriers are responsible for the DIBs at longer wavelengths, and have larger oscillator strengths, we found that the total column densities of the DIB carriers tend to decrease with increasing DIB wavelength. The candidate molecules and ions for the NIR DIBs are also discussed.

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Dissertations / Theses on the topic "Near IR high resolution astronomical spectrograph"

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SCHETTINO, GIULIA. "Optimization and astrophysical applications of ultra-high precision spectroscopic measurements." Doctoral thesis, 2012. http://hdl.handle.net/2158/609917.

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Conference papers on the topic "Near IR high resolution astronomical spectrograph"

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Zhao, Bo, and Jian Ge. "Optical design of a versatile FIRST high-resolution near-IR spectrograph." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean, Suzanne K. Ramsay, and Hideki Takami. SPIE, 2012. http://dx.doi.org/10.1117/12.926135.

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Jaffe, D. T., D. J. Mar, D. Warren, and P. R. Segura. "GMTNIRS: the high resolution near-IR spectrograph for the Giant Magellan Telescope." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean and Masanori Iye. SPIE, 2006. http://dx.doi.org/10.1117/12.672148.

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Ikeda, Yuji, Naoto Kobayashi, Sohei Kondo, Chikako Yasui, Kentaro Motohara, and Atsushi Minami. "WINERED: a warm near-infrared high-resolution spectrograph." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean and Masanori Iye. SPIE, 2006. http://dx.doi.org/10.1117/12.672665.

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Liang, Ming, R. R. Joyce, S. S. Eikenberry, K. H. Hinkle, G. P. Muller, Jian Ge, and David Sprayberry. "Optical design of the high-resolution near-infrared spectrograph." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean and Masanori Iye. SPIE, 2006. http://dx.doi.org/10.1117/12.671895.

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Hinkle, Kenneth H., Richard R. Joyce, and Joan R. Najita. "Design inputs for a high-performance high-resolution near-infrared spectrograph." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean, Suzanne K. Ramsay, and Hideki Takami. SPIE, 2010. http://dx.doi.org/10.1117/12.856285.

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Muller, G. P., E. A. Hileman, K. H. Hinkle, R. R. Joyce, M. Liang, D. Sprayberry, and S. S. Eikenberry. "Mechanical design of the Gemini high resolution near-infrared spectrograph." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean and Masanori Iye. SPIE, 2006. http://dx.doi.org/10.1117/12.672120.

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Origlia, L., E. Oliva, C. Baffa, G. Falcini, E. Giani, F. Massi, P. Montegriffo, et al. "High resolution near IR spectroscopy with GIANO-TNG." In SPIE Astronomical Telescopes + Instrumentation, edited by Suzanne K. Ramsay, Ian S. McLean, and Hideki Takami. SPIE, 2014. http://dx.doi.org/10.1117/12.2054743.

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D'Odorico, Sandro, Michael I. Andersen, Paolo Conconi, Vincenzo De Caprio, Bernard Delabre, Paolo Di Marcantonio, Hans Dekker, et al. "X-shooter: UV-to-IR intermediate-resolution high-efficiency spectrograph for the ESO VLT." In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2004. http://dx.doi.org/10.1117/12.550005.

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Oliva, E., and L. Origlia. "High-resolution near-IR spectroscopy: from 4m to 40m class telescopes." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean and Mark M. Casali. SPIE, 2008. http://dx.doi.org/10.1117/12.788821.

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Eikenberry, Stephen, Kenneth Hinkle, Dick Joyce, Ming Liang, Gary Muller, Ed Heileman, Jim French, et al. "Systems engineering and performance modeling of the Gemini High-Resolution Near-Infrared Spectrograph (HRNIRS)." In SPIE Astronomical Telescopes + Instrumentation, edited by Martin J. Cullum and George Z. Angeli. SPIE, 2006. http://dx.doi.org/10.1117/12.672368.

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