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Journal articles on the topic 'Star system spectroscopy'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Hinkle, Kenneth H., Stephen T. Ridgway, and Francis C. Fekel. "Infrared Spectroscopy of Multiple Star Systems." International Astronomical Union Colloquium 135 (1992): 149–51. http://dx.doi.org/10.1017/s0252921100006266.

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AbstractUp to this time infrared spectroscopy has been only occasionally used in binary star research due to both the insensitivity of infrared spectrographs and the difficulty of getting observing time on a limited number of spectrographs. However, infrared spectroscopy has a number of interesting applications in binary star research. We present an example of an application to the long-period symbiotic system CH Cyg. Due to the recent development of infrared arrays, infrared spectroscopy (1) is becoming available at a much larger number of telescopes and (2) in the 1.0-2.5 μm region is capabl

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2

Maíz Apellániz, J., R. H. Barbá, S. Simón-Díaz, et al. "Lucky Spectroscopy, an equivalent technique to Lucky Imaging." Astronomy & Astrophysics 615 (July 2018): A161. http://dx.doi.org/10.1051/0004-6361/201832885.

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Context. Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. Aims. We want to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. Methods. We obtained a large number of short long-slit spectroscopic exposures of five close binaries under good seeing conditions. We selected those with the best characteristics, extracted the spectra using multiple-profile fitting, and combined the results to derive spatially separated spectra. Results. We demonstrate the usefulness of Lucky Spectroscopy b

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Charles, P. A. "Black-Hole Systems: Optical Spectroscopy and IR Photometry." Symposium - International Astronomical Union 165 (1996): 341–50. http://dx.doi.org/10.1017/s0074180900055807.

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The X-ray transient systems have provided the first opportunities for detailed studies of the mass losing star in low-mass X-ray binaries. During X-ray quiescence the cool star is the dominant light source in the red and near-IR. Optical spectroscopy yields the mass function (itself a lower limit to the compact-object mass), the rotational broadening leads to the mass ratio, q (assuming only that the star fills its Roche lobe), and the IR ellipsoidal light curve gives the system inclination (for high q). In such cases, a complete solution to the system parameters is possible, and this has been

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Moffat, Anthony F. J. "Time-resolved optical-UV spectroscopy of colliding wind effects." Symposium - International Astronomical Union 193 (1999): 278–88. http://dx.doi.org/10.1017/s0074180900205548.

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It is in the ultraviolet-optical domain where the strongest known emission lines arise in hot star winds. In the case of hot-star binaries, culminating in the relatively common, strong-wind WR+O systems, similar line-emission is seen in the cooling flows downstream from the highly compressed, X-ray emitting heads of the bow shock regions produced when the two winds collide. Time-resolved UV-optical spectroscopy of these flows around a complete orbit can provide important constraints not only on the colliding wind process itself, but also on the winds and the orbit. Spectroscopic wind-wind coll

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Hajduk, Marcin, Peter A. M. van Hoof, and Albert A. Zijlstra. "GLMP 160 – the first [WR] star in a binary." Proceedings of the International Astronomical Union 7, S283 (2011): 382–83. http://dx.doi.org/10.1017/s1743921312011532.

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AbstractWe discuss the results of the search for [WR] central stars in binary systems. GLMP 160 is the first [WR] central star in a binary system known. We analyze photometry, spectroscopy and imaging of this system.

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Walton, N. A., J. R. Walsh, and S. R. Pottasch. "Imaging and Spectroscopy of Abell 63 (UU SGE)." Symposium - International Astronomical Union 155 (1993): 394. http://dx.doi.org/10.1017/s0074180900171839.

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UU Sge, the eclipsing binary central star (Bond et al, 1978) of the low-surface-brightness planetary nebula (PN) Abell 63, has been observed spectroscopically in the visible throughout its 11.2 hour period and especially during the minimum. A spectral determination of the binary system has been made. The primary hot central star is an ‘O’ type PN nucleus of temperature ≈40,000 K, consistent with the low excitation of the nebular spectrum (e.g. no He ii 4686Å nebular emission detected). From the spectrum at minimum light, the secondary star appears to be a cool dwarf star around G7. Measurement

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Skopal, A., D. Chochol, A. Vittone, and A. Mammano. "Photometric and Spectroscopic Variations of the Symbiotic Star EG Andromedae." International Astronomical Union Colloquium 103 (1988): 289–90. http://dx.doi.org/10.1017/s0252921100103665.

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EG And is a symbiotic binary system. The cool component is an M3 III star, the hot one is a subdwarf with temperature 60 250 K and luminosity 1.45 L⊙ (Boyarchuk, 1985). The eclipsing nature of the system suggested from UV spectroscopy by Oliversen et al. (1985) was confirmed photometrically by Chochol et al. (1987). The circular spectroscopic orbit of cool component determined by Oliversen et al. (1985) supposing the orbital period 470 days leads to f(m) = 3.2×10−2 M⊙ and detached configuration.

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Hummel, Christian A. "Imaging and Modeling of Double Stars with the Navy Prototype Optical Interferometer: a Continuation of the Mark III Double Star Program." International Astronomical Union Colloquium 170 (1999): 416–21. http://dx.doi.org/10.1017/s0252921100048855.

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AbstractWe present results from the new Navy Prototype Optical Interferometer (NPOI) – the orbit of the double star Mizar A and measurements of Matar – which are compared to an orbit determined with the predecessor of NPOI, the Mark III Interferometer. Uncertainties of the orbital inclination are between 0.1 and 0.3 degrees; those of the semi-major axis are less than 0.5 percent. We determine the component masses and other parameters of the double star system, including relative photometry, directly through a fit to a combination of interferometric and spectroscopic data. Algorithms were devel

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Hinkle, Kenneth H., Francis C. Fekel, Richard R. Joyce, Joanna Mikołajewska, Cezary Gałan, and Thomas Lebzelter. "Infrared Spectroscopy of Symbiotic Stars. XII. The Neutron Star SyXB System 4U 1700+24 = V934 Herculis." Astrophysical Journal 872, no. 1 (2019): 43. http://dx.doi.org/10.3847/1538-4357/aafba5.

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10

Davis, John. "Overview of Multiple–Aperture Interferometry Binary Star Results from the Southern Hemisphere." Proceedings of the International Astronomical Union 2, S240 (2006): 45–53. http://dx.doi.org/10.1017/s174392130700378x.

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AbstractThe first multiple-aperture interferometric study of a binary system, in which the power of combining interferometric and spectroscopic data was demonstrated, was made from the Southern Hemisphere. The observations of α Vir with the Narrabri Stellar Intensity Interferometer (NSII) were combined with spectroscopic and photometric data to yield the mass, radius and luminosity of the primary as well as an accurate distance to the system. The NSII also revealed a number of stars, previously thought to be single, to be binary systems. Several of these systems have subsequently been shown to

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Kochukhov, O., C. Johnston, J. Labadie-Bartz, et al. "V772 Cas: an ellipsoidal HgMn star in an eclipsing binary." Monthly Notices of the Royal Astronomical Society 500, no. 2 (2020): 2577–89. http://dx.doi.org/10.1093/mnras/staa3472.

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ABSTRACT The late B-type star V772 Cas (HD 10260) was previously suspected to be a rare example of a magnetic chemically peculiar star in an eclipsing binary system. Photometric observations of this star obtained by the TESS satellite show clear eclipses with a period of 5.0137 d accompanied by a significant out-of-eclipse variation with the same period. High-resolution spectroscopy reveals V772 Cas to be an SB1 system, with the primary component rotating about a factor two slower than the orbital period and showing chemical peculiarities typical of non-magnetic HgMn chemically peculiar stars.

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P. Huenemoerder, David, Bram Boroson, Norbert S. Schulz, et al. "Stellar Coronal Spectroscopy with the Chandra HETGS." Symposium - International Astronomical Union 219 (2004): 238–42. http://dx.doi.org/10.1017/s0074180900182178.

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Spectroscopy with the Chandra High Energy Transmission Grating Spectrometer (HETGS) provides details on X-ray emission and activity from young and cool stars through resolution of emission lines from a variety of ions. We are beginning to see trends in activity regarding abundances, emission measures, and variability. Here we contrast spectra of TV Crt, a weak-lined T Tauri star (WTT), with TW Hya, a Classical T Tauri star (CTT). TV Crt has a spectrum more like magnetic activity driven coronae, relative to the TW Hya spectrum, which we have interpreted as due to accretion-produced X-rays. We h

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Robertson, J. G., T. R. Bedding, C. Aerts, C. Waelkens, R. G. Marson, and J. R. Barton. "Interferometry and spectroscopy of Cen: a Cephei star in a binary system." Monthly Notices of the Royal Astronomical Society 302, no. 2 (1999): 245–52. http://dx.doi.org/10.1046/j.1365-8711.1999.02068.x.

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Herath, Mahesh, Tobias C. Hinse, John H. Livingston, et al. "Two temperate sub-Neptunes transiting the star EPIC 212737443." Monthly Notices of the Royal Astronomical Society 488, no. 1 (2019): 536–46. http://dx.doi.org/10.1093/mnras/stz1641.

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ABSTRACT We report the validation of a new planetary system around the K3 star EPIC 212737443 using a combination of K2 photometry, follow-up high-resolution imaging and spectroscopy. The system consists of two sub-Neptune sized transiting planets with radii of 2.6R⊕ and 2.7R⊕, with orbital periods of 13.6 and 65.5 d, equilibrium temperatures of 536 and 316 K, respectively. In the context of validated K2 systems, the outer planet has the longest precisely measured orbital period, as well as the lowest equilibrium temperature for a planet orbiting a star of spectral type earlier than M. The two

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van den Besselaar, E. J. M., R. Greimel, L. Morales-Rueda, et al. "DE CVn: A Bright, Eclipsing Red Dwarf – White Dwarf Binary." Proceedings of the International Astronomical Union 2, S240 (2006): 105–8. http://dx.doi.org/10.1017/s1743921307003882.

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AbstractDE CVn is a relatively unstudied eclipsing binary where one of the components is an M dwarf and the other is a white dwarf. Its brightness makes it an ideal system for a detailed study in the context of common-envelope evolution of a detached white dwarf – red dwarf binary with a relatively short orbital period (∼8.7 hours). We present a detailed study of the basic parameters (e.g. orbital period, components' masses and spectral types) for this system from photometric and spectroscopic studies. The eclipses observed during several photometric observing runs were used to derive the ephe

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Murgas, F., E. Pallé, H. Parviainen, et al. "The GTC exoplanet transit spectroscopy survey." Astronomy & Astrophysics 605 (September 2017): A114. http://dx.doi.org/10.1051/0004-6361/201730937.

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Context. Transiting planets offer an excellent opportunity for characterizing the atmospheres of extrasolar planets under very different conditions from those found in our solar system. Aims. We are currently carrying out a ground-based survey to obtain the transmission spectra of several extrasolar planets using the 10 m Gran Telescopio Canarias. In this paper we investigate the extrasolar planet WASP-48b, a hot Jupiter orbiting around an F-type star with a period of 2.14 days. Methods. We obtained long-slit optical spectroscopy of one transit of WASP-48b with the Optical System for Imaging a

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Chandar, Rupali, Luciana Bianchi, Holland C. Ford, and Ata Sarajedini. "Kinematics of Star Clusters in M33: Distinct Populations." Symposium - International Astronomical Union 207 (2002): 160–62. http://dx.doi.org/10.1017/s0074180900223619.

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We analyse star cluster properties in the nearby spiral galaxy M33, combining our extensive HST WFPC2 photometry and ground-based follow up spectroscopy. These data show that cluster velocity dispersion increases with age. Simulations comparing synthetic disk and halo populations with observations indicate a composite disk/halo system for the old M33 clusters. The best fit fraction of 85 ± 5% halo plus 15 ± 5% disk differs from that found in the Milky Way, where ∼ 30% of the globular clusters are metal rich objects associated with the bulge and/or thick disk. Spectroscopic line indices for a h

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18

Mikolajewski, M., T. Tomov, and J. Mikolajewska. "Optical Spectroscopy of CH Cygni in 1985/86." International Astronomical Union Colloquium 93 (1987): 733–45. http://dx.doi.org/10.1017/s0252921100105615.

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AbstractSome arguments for the explanation of the spectroscopic and photometric behavior of CH Cyg in terms of an eclipsing binary with P=5700 days, consisting of M6 III star and an accreting white dwarf, are presented. Physical and geometrical parameters of the system have been estimated and discussed.

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Stoyanov, K. A., K. Iłkiewicz, G. J. M. Luna, et al. "Optical spectroscopy and X-ray observations of the D-type symbiotic star EF Aql." Monthly Notices of the Royal Astronomical Society 495, no. 1 (2020): 1461–67. http://dx.doi.org/10.1093/mnras/staa1310.

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ABSTRACT We performed high-resolution optical spectroscopy and X-ray observations of the recently identified Mira-type symbiotic star EF Aql. Based on high-resolution optical spectroscopy obtained with the Southern African Large Telescope (SALT), we determine the temperature (∼55 000 K) and the luminosity (∼5.3 L⊙) of the hot component in the system. The heliocentric radial velocities of the emission lines in the spectra reveal possible stratification of the chemical elements. We also estimate the mass-loss rate of the Mira donor star. Our Swift observation did not detect EF Aql in X-rays. The

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Frémat, Y., P. Lampens, H. Hensberge, et al. "High resolution spectroscopy of the triple system 20 Leo." International Astronomical Union Colloquium 193 (2004): 395–98. http://dx.doi.org/10.1017/s0252921100011015.

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Abstract20 Leo is a spectroscopic triple system composed of 3 very similar stars, one of which seems to be aδSct star. Observations at high spectral and high time resolution have been obtained at the Observatoire de Haute Provence with the ELODIE spectrograph on the 1.9-m telescope. The spectra were taken during 7 nights in 2003 January and cover the whole optical domain from 3900 to 6800 Å. We used a Fourier transform technique recently developed by P. Hadrava to disentangle the combined spectrum. Application of the method allows the derivation of radial velocities at all orbital phases (even

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Surace, C., J. Hecquet, and M. Auriere. "Spectroscopic Study of NGC 6119 - NGC 6120 System." Symposium - International Astronomical Union 171 (1996): 448. http://dx.doi.org/10.1017/s0074180900233664.

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NGC6119 and NGC6120 have been listed in Kiso catalog (Takase et al., 1987) as Sc and Irr galaxies. They have been selected by their clumpy features in order to investigate their nature and star formation history using slit spectroscopy. They have similar systemic velocities (respectively 9215 and 9200 km ·s–1) and seem to be members of a low gravitational interacting system of 4 galaxies (with MCG-6-36-30 and NGC6122).

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Piccioni, A., C. Bartolini, S. Bernabei, S. Galleti, A. Guarnieri, and G. Valentini. "Photometry and Spectroscopy of X Per During the Years 1996-1999." International Astronomical Union Colloquium 175 (2000): 585–88. http://dx.doi.org/10.1017/s0252921100056578.

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AbstractUBVRI photoelectric monitoring of the Be star X Per, a transient X-ray binary, during the last four years, along with some optical spectra are presented and briefly discussed in the context of the long term behaviour of the system.

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Bourrier, V., X. Dumusque, C. Dorn, et al. "The 55 Cancri system reassessed." Astronomy & Astrophysics 619 (October 30, 2018): A1. http://dx.doi.org/10.1051/0004-6361/201833154.

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Orbiting a bright, nearby star the 55 Cnc system offers a rare opportunity to study a multiplanet system that has a wide range of planetary masses and orbital distances. Using two decades of photometry and spectroscopy data, we have measured the rotation of the host star and its solar-like magnetic cycle. Accounting for this cycle in our velocimetric analysis of the system allows us to revise the properties of the outermost giant planet and its four planetary companions. The innermost planet 55 Cnc e is an unusually close-in super-Earth, whose transits have allowed for detailed follow-up studi

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Armas Padilla, M., T. Muñoz-Darias, F. Jiménez-Ibarra, et al. "Optical spectroscopy of 4U 1812–12." Astronomy & Astrophysics 644 (December 2020): A63. http://dx.doi.org/10.1051/0004-6361/202038997.

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The persistent low-luminosity neutron star X-ray binary 4U 1812−12 is a potential member of the scarce family of ultra-compact systems. We performed deep photometric and spectroscopic optical observations with the 10.4 m Gran Telescopio Canarias in order to investigate the chemical composition of the accreted plasma, which is a proxy for the donor star class. We detect a faint optical counterpart (g ∼ 25, r ∼ 23) that is located in the background of the outskirts of the Sharpless 54 H II region, whose characteristic nebular lines superimpose on the X-ray binary spectrum. Once this is corrected

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Zieba, S., K. Zwintz, M. A. Kenworthy та G. M. Kennedy. "Transiting exocomets detected in broadband light by TESS in the β Pictoris system". Astronomy & Astrophysics 625 (травень 2019): L13. http://dx.doi.org/10.1051/0004-6361/201935552.

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Aims. We search for signs of falling evaporating bodies (FEBs, also known as exocomets) in photometric time series obtained for β Pictoris after fitting and removing its δ Scuti-type pulsation frequencies. Methods. Using photometric data obtained by the TESS satellite we determined the pulsational properties of the exoplanet host star β Pictoris through frequency analysis. We then pre-whitened the 54 identified δ Scuti p-modes and investigated the residual photometric time series for the presence of FEBs. Results. We identify three distinct dipping events in the light curve of β Pictoris over

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Lennon, D. J., J. Maíz Apellániz, A. Irrgang, et al. "Hubble spectroscopy of LB-1: Comparison with B+black-hole and Be+stripped-star models." Astronomy & Astrophysics 649 (May 2021): A167. http://dx.doi.org/10.1051/0004-6361/202040253.

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Context. LB-1 (alias ALS 8775) has been proposed as either an X-ray dim B-type star plus black hole (B+BH) binary or a Be star plus an inflated stripped star (Be+Bstr) binary. The latter hypothesis contingent upon the detection and characterization of the hidden broad-lined star in a composite optical spectrum. Aims. Our study is aimed at testing the published B+BH (single star) and Be+Bstr (binary star) models using a flux-calibrated UV-optical-IR spectrum. Methods. The Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST) was used to obtain a flux-calibrated s

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Echevarría, J., F. Diego, M. Tapia, and R. Costero. "Echelle-Mepsicron Time-Resolved Spectroscopy of the Dwarf Nova SS Cygni." International Astronomical Union Colloquium 93 (1987): 111. http://dx.doi.org/10.1017/s0252921100104701.

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AbstractHigh dispersion time-resolved spectrograms of the dwarf nova SS Cygni, obtained with the Echelle-Mepsicron system, show double peaked emission lines with a complex profile. The intensity of the Hβ line appears to be modulated by the orbital period. Radial velocity measurements of the wings of Hβ and of the absorption line system of the late-type star yield semiamplitude values of Kem = 101 ± 6 km s−1 and Kab = 151 ± 7 km s−1, respectively. Radial velocity measurements of the blue and red peaks and of the central absorption of Hβ reveal a synchronous movement with the broad wings, altho

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Murgas, F., G. Chen, E. Pallé, L. Nortmann, and G. Nowak. "The GTC exoplanet transit spectroscopy survey." Astronomy & Astrophysics 622 (February 2019): A172. http://dx.doi.org/10.1051/0004-6361/201834063.

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Context. Rayleigh scattering in a hydrogen-dominated exoplanet atmosphere can be detected using ground- or space-based telescopes. However, stellar activity in the form of spots can mimic Rayleigh scattering in the observed transmission spectrum. Quantifying this phenomena is key to our correct interpretation of exoplanet atmospheric properties. Aims. We use the ten-meter Gran Telescopio Canarias (GTC) telescope to carry out a ground-based transmission spectra survey of extrasolar planets to characterize their atmospheres. In this paper we investigate the exoplanet HAT-P-11b, a Neptune-sized p

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Yuliana, Fitri, Zulkarnain Zulkarnain та Hakim Luthfi Malasan. "PENENTUAN KOMPOSISI KIMIAWI ATMOSFER DAN TEMPERATUR EFEKTIF PADA BINTANG VEGA (α Lyr) DENGAN MENGGUNAKAN METODE SPEKTROSKOPI ABSORPSI". Komunikasi Fisika Indonesia 16, № 2 (2019): 96. http://dx.doi.org/10.31258/jkfi.16.2.96-102.

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The star spectrum is an information which is though to be a map of the star. The shape of the spectral line actually shows the nature of the star atmosphere, which is the only part researcher can be reached. The intensities of spectral lines will determine the chemical composition of the stars contained in the atmospheres of the stars. The approach used to determine the chemical composition and the effective temperature of the star is spectroscopy. The spectroscopy method had been done in this study using the GAO-ITB RTS telescope system which consisting of the Celestron C11 telescope, NEO-R 1

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Hareter, Markus, та Margit Paparó. "CoRoT target HD 51844: a δ Scuti star in a binary system with periastron brightening". Proceedings of the International Astronomical Union 9, S301 (2013): 59–62. http://dx.doi.org/10.1017/s1743921313014087.

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AbstractThe star HD 51844 was observed in the CoRoT LRa02 as a target in the seismology field, which turned out to be an SB2 system. The 117-day light curve revealed δ Scuti pulsations in the range of 6 to 15 d−1 where four frequencies have amplitudes larger than 1.4 mmag, and a rich frequency spectrum with amplitudes lower than 0.6 mmag. Additionally, the light curve exhibits a 3-mmag brightening event recurring every 33.5 days with a duration of about 5 days. The radial velocities from spectroscopy confirmed that the star is an eccentric binary system with nearly identical masses and physica

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Lane, Benjamin F., Matthew W. Muterspaugh, R. F. Griffin, et al. "THE ORBITS OF THE TRIPLE-STAR SYSTEM 1 GEMINORUM FROM PHASES DIFFERENTIAL ASTROMETRY AND SPECTROSCOPY." Astrophysical Journal 783, no. 1 (2014): 3. http://dx.doi.org/10.1088/0004-637x/783/1/3.

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Holberg, J. B., S. L. Casewell, Howard E. Bond, M. R. Burleigh, and M. A. Barstow. "Hubble Space Telescope imaging and spectroscopy of the sirius-like triple star system HD 217411." Monthly Notices of the Royal Astronomical Society 444, no. 3 (2014): 2022–30. http://dx.doi.org/10.1093/mnras/stu1431.

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Kunovac Hodžić, Vedad, Amaury H. M. J. Triaud, David V. Martin, et al. "The EBLM project – VII. Spin–orbit alignment for the circumbinary planet host EBLM J0608-59 A/TOI-1338 A." Monthly Notices of the Royal Astronomical Society 497, no. 2 (2020): 1627–33. http://dx.doi.org/10.1093/mnras/staa2071.

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ABSTRACT A dozen short-period detached binaries are known to host transiting circumbinary planets. In all circumbinary systems so far, the planetary and binary orbits are aligned within a couple of degrees. However, the obliquity of the primary star, which is an important tracer of their formation, evolution, and tidal history, has only been measured in one circumbinary system until now. EBLM J0608-59/TOI-1338 is a low-mass eclipsing binary system with a recently discovered circumbinary planet identified by TESS. Here, we perform high-resolution spectroscopy during primary eclipse to measure t

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Mennickent, Ronald E., Darek Graczyk, Zbigniew Kołaczkowski, Gabriela Michalska, Daniela Barría, and Ewa Niemczura. "Optical spectroscopy of DPVs and the case of LP Ara." Proceedings of the International Astronomical Union 6, S272 (2010): 527–28. http://dx.doi.org/10.1017/s1743921311011306.

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AbstractWe present preliminary results of our spectroscopic campaign of a group of intermediate mass interacting binaries dubbed “Double Periodic Variables” (DPVs), characterized by orbital light curves and additional long photometric cycles recurring roughly after 33 orbital periods (Mennickent et al. 2003, 2005). They have been interpreted as interacting, semi-detached binaries showing cycles of mass loss into the interstellar medium (Mennickent et al. 2008, Mennickent & Kołaczkowski 2009). High resolution Balmer and helium line profiles of DPVs can be interpreted in terms of mass flows

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Drinkwater, M. J., J. B. Jones, M. D. Gregg, and S. Phillipps. "Compact Stellar Systems in the Fornax Cluster: Super-massive Star Clusters or Extremely Compact Dwarf Galaxies?" Publications of the Astronomical Society of Australia 17, no. 3 (2000): 227–33. http://dx.doi.org/10.1071/as00034.

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AbstractWe describe a population of compact objects in the centre of the Fornax Cluster which were discovered as part of our 2dF Fornax Spectroscopic Survey. These objects have spectra typical of old stellar systems, but are unresolved on photographic sky survey plates. They have absolute magnitudes −13 < MB < −11, so they are 10 times more luminous than any Galactic globular clusters, but fainter than any known compact dwarf galaxies. These objects are all within 30 arcminutes of the central galaxy of the cluster, NGC 1399, but are distributed over larger radii than the globular cluster

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Pyun, Jeffrey, Ian Rees, Jean M. J. Fréchet, and Craig J. Hawker. "Evaluating the Effect of Termination by Chain - Chain Coupling in Living Free-Radical Polymerizations." Australian Journal of Chemistry 56, no. 8 (2003): 775. http://dx.doi.org/10.1071/ch03041.

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A novel approach based on the reaction of multifunctional star polymers with chromophore-labelled linear polymers is presented for evaluating the extent of termination by chain–chain coupling during living free-radical polymerizations. A mixed initiating system consisting of an unlabelled, multifunctional initiator and an excess of a monofunctional alkoxyamine initiator containing a chromophore, such as pyrene, is used to initiate the living polymerization of vinyl monomers leading to a mixture of star and linear polymers. The occurrence of chain–chain coupling is readily identified and quanti

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Yoshida, M., Y. Shimizu, H. Koyano, et al. "Tridimensional Observations of Nearby Active Galaxies Using OAO Spectronebulagraph." International Astronomical Union Colloquium 149 (1995): 207–8. http://dx.doi.org/10.1017/s0252921100022971.

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We developed a slit-scanning type 3D-spectroscopic system named as Spectronebulagraph (hereafter SNG; Kosugi et al. 1994) at Okayama Astrophysical Observatory. A detailed description about SNG is presented by Ohtani et al. elsewhere in this colloquium. We present here the results of the 3D-spectroscopy of four nearby active galaxies by using SNG.This nearby (at distance of 5.4 Mpc) Magellanic irregular galaxy has many H II regions in its main body suggesting violent star-formation activity. We performed tridimensional observations of NGC 4449 using SNG in order to obtain detailed kinematic str

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Shenar, T., R. Hainich, H. Todt, et al. "The shortest-period Wolf-Rayet binary in the Small Magellanic Cloud: Part of a high-order multiple system." Astronomy & Astrophysics 616 (August 2018): A103. http://dx.doi.org/10.1051/0004-6361/201833006.

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Context. SMC AB 6 is the shortest-period (P = 6.5 d) Wolf-Rayet (WR) binary in the Small Magellanic Cloud. This binary is therefore a key system in the study of binary interaction and formation of WR stars at low metallicity. The WR component in AB 6 was previously found to be very luminous (log L = 6.3 [L⊙]) compared to its reported orbital mass (≈8 M⊙), placing it significantly above the Eddington limit. Aims. Through spectroscopy and orbital analysis of newly acquired optical data taken with the Ultraviolet and Visual Echelle Spectrograph (UVES), we aim to understand the peculiar results re

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Armas Padilla, M., and E. López-Navas. "On the ultra-compact nature of the neutron star system 1RXS J170854.4−321857: insights from X-ray spectroscopy." Monthly Notices of the Royal Astronomical Society 488, no. 4 (2019): 5014–19. http://dx.doi.org/10.1093/mnras/stz2004.

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ABSTRACT The relatively small family of ultra-compact X-ray binary systems is of great interest for many areas of astrophysics. We report on a detailed X-ray spectral study of the persistent neutron star low-mass X-ray binary 1RXS J170854.4−321857. We analysed two XMM–Newton observations obtained in late 2004 and early 2005 when, in agreement with previous studies, the system displayed an X-ray luminosity (0.5–10 keV) of ${\sim} 1\times 10^{36}\, \mathrm{erg~s}^{-1}$. The spectrum can be described by a Comptonized emission component with Γ ∼ 1.9 and a distribution of seed photons with a temper

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Palle, E., M. Oshagh, N. Casasayas-Barris, et al. "Transmission spectroscopy and Rossiter-McLaughlin measurements of the young Neptune orbiting AU Mic." Astronomy & Astrophysics 643 (October 28, 2020): A25. http://dx.doi.org/10.1051/0004-6361/202038583.

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AU Mic b is a Neptune-sized planet on an 8.47-day orbit around the nearest pre-main sequence (~20 Myr) star to the Sun, the bright (V = 8.81) M dwarf AU Mic. The planet was preliminary detected in Doppler radial velocity time series and recently confirmed to be transiting with data from the TESS mission. AU Mic b is likely to be cooling and contracting and might be accompanied by a second, more massive planet, in an outer orbit. Here, we present the observations of the transit of AU Mic b using ESPRESSO on the Very Large Telescope. We obtained a high-resolution time series of spectra to measur

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Mengel, Sabine, Niranjan Thatte, Matthew Lehnert, and Reinhard Genzel. "Star Formation in NGC 4038/4039." Symposium - International Astronomical Union 205 (2001): 206–7. http://dx.doi.org/10.1017/s0074180900220986.

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We performed near infrared integral field spectroscopy of several star clusters and the nuclei of the prototypical merger NGC 4038/39 (“The Antennae”). Near infrared (NIR) images covered both galaxies. The collision of the two gas-rich spiral galaxies has triggered a starburst obvious from a large number of young star clusters. ISO data suggest that the most active star formation occurs in the region where the two galaxy disks overlap. A significant fraction of the total bolometric luminosity of the system is produced there. Since this region is heavily extincted in the optical, the investigat

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Ciocan, B. I., B. L. Ziegler, M. Verdugo, et al. "The VLT-MUSE and ALMA view of the MACS 1931.8-2635 brightest cluster galaxy." Astronomy & Astrophysics 649 (May 2021): A23. http://dx.doi.org/10.1051/0004-6361/202040010.

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We reveal the importance of ongoing in situ star formation in the brightest cluster galaxy (BCG) in the massive cool-core CLASH cluster MACS 1931.8-2635 at a redshift of z = 0.35 by analysing archival VLT-MUSE optical integral field spectroscopy. Using a multi-wavelength approach, we assessed the stellar and warm ionised medium components, which were spatially resolved by the VLT-MUSE spectroscopy, and linked them to the molecular gas by incorporating sub-mm ALMA observations. We measured the fluxes of strong emission lines such as: [O II] λ3727, Hβ, [O III] λ5007, Hα, [N II] λ 6584, and [S II

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Kerzendorf, Wolfgang E. "Type Ia Progenitor Hunt in Ancient Remnants." Proceedings of the International Astronomical Union 7, S281 (2011): 326–30. http://dx.doi.org/10.1017/s174392131201530x.

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AbstractThere is broad agreement that the stars which explode as Type Ia supernovae are white dwarfs. They have accreted material in a binary system until they are near the Chandrasekhar mass and detonate/deflagrate. The two main scenarios for this accretion process are merging with a companion white dwarf (double degenerate scenario), or accretion from a main-sequence to red giant donor (single degenerate scenario). The donor star survives post-explosion and would provide substantial evidence for the single degenerate scenario, if found. Our team is analyzing stars in close proximity to Galac

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Hoeijmakers, H. J., H. Schwarz, I. A. G. Snellen, et al. "Medium-resolution integral-field spectroscopy for high-contrast exoplanet imaging." Astronomy & Astrophysics 617 (September 2018): A144. http://dx.doi.org/10.1051/0004-6361/201832902.

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Context. Angular differential imaging (ADI) and spectral differential imaging (SDI) are well-established high-contrast imaging techniques, but their application is challenging for companions at small angular separations from their host stars. Aims. The aim of this paper is to investigate to what extent adaptive-optics assisted, medium-resolution (R ~ 5000) integral field spectrographs (IFS) can be used to directly detect the absorption of molecular species in the spectra of planets and substellar companions when these are not present in the spectrum of the star. Methods. We analysed archival d

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Murphy, Simon J., Tanda Li, Sanjay Sekaran та ін. "A binary with a δ Scuti star and an oscillating red giant: orbit and asteroseismology of KIC 9773821". Monthly Notices of the Royal Astronomical Society 505, № 2 (2021): 2336–48. http://dx.doi.org/10.1093/mnras/stab1436.

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ABSTRACT We study the δ Scuti – red giant (RG) binary KIC 9773821, the first double-pulsator binary of its kind. It was observed by Kepler during its 4-yr mission. Our aims are to ascertain whether the system is bound, rather than a chance alignment, and to identify the evolutionary state of the RG via asteroseismology. An extension of these aims is to determine a dynamical mass and an age prior for a δ Sct star, which may permit mode identification via further asteroseismic modelling. We determine spectroscopic parameters and radial velocities (RVs) for the RG component using HERMES@Mercator

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Shahbaz, T., M. Linares, P. Rodríguez-Gil, and J. Casares. "The binary millisecond pulsar PSR J1023+0038 – II. Optical spectroscopy." Monthly Notices of the Royal Astronomical Society 488, no. 1 (2019): 198–212. http://dx.doi.org/10.1093/mnras/stz1652.

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ABSTRACT We present time-resolved optical spectroscopy of the ‘redback’ binary millisecond pulsar system PSR J1023+0038 during both its radio pulsar (2009) and accretion disc states (2014 and 2016). We provide observational evidence for the companion star being heated during the disc state. We observe a spectral type change along the orbit, from ∼G5 to ∼F6 at the secondary star’s superior and inferior conjunction, respectively, and find that the corresponding irradiating luminosity can be powered by the high-energy accretion luminosity or the spin-down luminosity of the neutron star. We determ

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Karl, Martina, Oliver Pfuhl, Frank Eisenhauer, et al. "Multiple star systems in the Orion nebula." Astronomy & Astrophysics 620 (December 2018): A116. http://dx.doi.org/10.1051/0004-6361/201833575.

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This work presents an interferometric study of the massive-binary fraction in the Orion Trapezium cluster with the recently comissioned GRAVITY instrument. We observed a total of 16 stars of mainly OB spectral type. We find three previously unknown companions for θ1 Ori B, θ2 Ori B, and θ2 Ori C. We determined a separation for the previously suspected companion of NU Ori. We confirm four companions for θ1 Ori A, θ1 Ori C, θ1 Ori D, and θ2 Ori A, all with substantially improved astrometry and photometric mass estimates. We refined the orbit of the eccentric high-mass binary θ1 Ori C and we are

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Stencel, Robert E. "Evidence for a Precessing Disk in the Extreme Binary ϵ Aurigae". Proceedings of the International Astronomical Union 2, S240 (2006): 202–4. http://dx.doi.org/10.1017/s1743921307004024.

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AbstractAmong the longest known eclipse durations and binary periods is that of the star ϵ Aurigae, which exhibits 2-year long eclipses every 27.1 years. Oddly, the nature of the secondary in the system continues to elude ready identification. In 1965, Huang proposed a massive disk as the eclipsing body, and study of the 1984 eclipse led Lissauer and Backman to suggest an embedded B star binary in the disk to maintain it. A collaboration of observers allows me to present recent optical photometry and spectroscopy, near-IR spectroscopy and Spitzer space telescope IRS and MIPS observations of ϵ

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Mason, Brian D., William I. Hartkopf, Dimitri Pourbaix, Colin D. Scarfe, Marion Schmitz, and Andrei A. Tokovinin. "DIVISION IV / COMMISSION 26 / WORKING GROUP BINARY AND MULTIPLE SYSTEM NOMENCLATURE." Proceedings of the International Astronomical Union 4, T27A (2008): 207–8. http://dx.doi.org/10.1017/s1743921308025520.

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The Working Group on Binary and Multiple System Nomenclature was formed within Commission 26 following Special Session 3 held during the 2003 Sydney General Assembly. Its purpose is to create the Washington Multiplicity Catalog, a comprehensive database first introduced at a multi-commission meeting at the IAU XXIV General Assembly in Manchester, 2000. Data are being compiled from the US Naval Observatory visual binary catalogs and supplemented with binary and multiple star information from other sources to include but not limited to spectroscopy, photometry, eclipsing and interacting system,

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Maíz Apellániz, J., E. Trigueros Páez, I. Negueruela, et al. "MONOS: Multiplicity Of Northern O-type Spectroscopic systems." Astronomy & Astrophysics 626 (June 2019): A20. http://dx.doi.org/10.1051/0004-6361/201935359.

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Context. Multiplicity in massive stars is key to understanding the chemical and dynamical evolution of galaxies. Among massive stars, those of O type play a crucial role due to their high masses and short lifetimes. Aims. MONOS (Multiplicity Of Northern O-type Spectroscopic systems) is a project designed to collect information and study O-type spectroscopic binaries with δ > −20°. In this first paper we describe the sample and provide spectral classifications and additional information for objects with previous spectroscopic and/or eclipsing binary orbits. In future papers we will test the

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