Publications
182 results found
Meikle W, Varani G, Spyromilio J, et al., 1991, Direct Observation of 56/CO Decay in Supernova 1987A, Supernovae
Spyromilio J, Meikle WPS, Allen DA, 1991, Spectral Line Profiles of Iron and Nickel in Supernova 1987A, Supernovae
Cumming R, Meikle WPS, Spyromilio J, et al., 1991, Supernova 1987A in the Large Magellanic Cloud, IAU Circular, 5156
R. Cumming and P. Meikle, Imperial College, London; and J. Spyromilio and D. Allen, Anglo-Australian Observatory, report "Echelle spectroscopy (resolution 40 000) of the circumstellar H-alpha emission from SN 1987A was performed at the Anglo-Australian Telescope on 1990 Dec. 22. A broad pedestal with FWHM about 150 km/s has appeared beneath the strong, narrow line (FWHM 30 km/s) and contributes about 30 percent of the line flux. There is no broad component to the neighboring [N II] emission, and similar spectra taken 53 days earlier (in better seeing) show no pedestal to any of the three lines. Preliminary analysis of spatially-separated spectra indicates that the broad component is strongest 1" east of the supernova. If the pedestal arises from interaction of the fast-moving ejecta with circumstellar material shed by the progenitor then it may evolve rapidly."
VARANI GF, MEIKLE WPS, SPYROMILIO J, et al., 1990, DIRECT OBSERVATION OF RADIOACTIVE COBALT DECAY IN SUPERNOVA-1987A, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 245, Pages: 570-576, ISSN: 0035-8711
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- Citations: 54
SPYROMILIO J, MEIKLE WPS, ALLEN DA, 1990, SPECTRAL-LINE PROFILES OF IRON AND NICKEL IN SUPERNOVA 1987A - EVIDENCE FOR A FRAGMENTED NICKEL BUBBLE, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 242, Pages: 669-673, ISSN: 0035-8711
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- Citations: 78
ALLEN DA, MEIKLE WPS, SPYROMILIO J, 1989, HELIUM ABUNDANCE AND ASYMMETRY IN THE WIND FROM THE PRECURSOR TO SUPERNOVA 1987A, NATURE, Vol: 342, Pages: 403-405, ISSN: 0028-0836
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- Citations: 20
Spyromilio J, Whitelock P, Meikle WPS, et al., 1989, V745 Scorpii, IAU Circular, 4885
J. Spyromilio and P. Whitelock, Anglo-Australian Observatory; P. Meikle and G. Varani, Imperial College, London; and M. Feast, South African Astronomical Observatory, telex: "Spectra (resolution 500) of V745 Sco were obtained at the Anglo-Australian Telescope in the J, K, and L' windows on Oct. 11. The spectra show strong He (1083 nm) and weaker Paschen beta and Brackett gamma, all in emission. The continuum in the J window rises toward longer wavelengths. The first overtone of CO is strong in absorption and presumably results from the companion star, possibly an M star (cf. IAUC 4844). The L' spectrum is approximately flat and featureless but of poorer signal-to-noise ratio. Photometry at SAAO yields: Aug. 28, J = 9.98, H = 8.74, K = 8.20, L = 7.51; Oct. 17, 9.99, 8.71, 8.23, 7.79."
Spyromilio J, Meikle WPS, Learner RCM, et al., 1989, Carbon monoxide in Supernova 1987a, Infrared Spectroscopy in Astronomy
Meikle W, 1989, Infrared spectroscopy of supernova 1987a, Infrared Spectroscopy in Astronomy
MEIKLE WPS, ALLEN DA, SPYROMILIO J, et al., 1989, SPECTROSCOPY OF SUPERNOVA 1987A AT 1-5 MU-M .1. THE 1ST YEAR, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 238, Pages: 193-223, ISSN: 0035-8711
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- Citations: 105
Allen DA, Meikle WPS, Spyromilio J, 1989, Supernova 1987A in the Large Magellanic Cloud, IAU Circulars, 4747
D. Allen, Anglo-Australian Observatory; and P. Meikle and J. Spyromilio, Imperial College, London, communicate: "We obtained observations, using an infrared spectrometer (FIGS) on the Anglo-Australian Telescope, of the 1083.0-nm He I line in SN 1987A. A narrow component, unresolved at resolution 300 km/s, has been present since at least 1988 Sept. with little change in intensity, and it now accounts for almost half the total line flux. On Feb. 28 the narrow component was found to arise predominently in a compact blob about 0".8 from the supernova at position angle 200 +/- 15 deg. A weaker, more diffuse component is also suspected to the north of the supernova. The narrow line most plausibly arises from excitation by the initial ultraviolet flash of a highly asymmetric progenitor wind. The position angle agrees with that of the velocity gradient measured in similar optical lines (IAUC 4739)."
GRAHAM JR, MEIKLE WPS, LONGMORE AJ, et al., 1988, THE INFRARED LIGHT CURVES AND COLORS OF SN-1984A, ASTROPHYSICAL JOURNAL, Vol: 333, Pages: 743-748, ISSN: 0004-637X
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- Citations: 5
ELIAS JH, GREGORY B, PHILLIPS MM, et al., 1988, LINE IDENTIFICATIONS IN THE INFRARED-SPECTRUM OF SN-1987A, ASTROPHYSICAL JOURNAL, Vol: 331, Pages: L9-L13, ISSN: 0004-637X
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- Citations: 33
SPYROMILIO J, MEIKLE WPS, LEARNER RCM, et al., 1988, CARBON-MONOXIDE IN SUPERNOVA-1987A, NATURE, Vol: 334, Pages: 327-329, ISSN: 0028-0836
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- Citations: 92
WRIGHT GS, JOSEPH RD, ROBERTSON NA, et al., 1988, RECENT STAR FORMATION IN INTERACTING GALAXIES .3. EVIDENCE FROM MID-INFRARED PHOTOMETRY, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 233, Pages: 1-23, ISSN: 0035-8711
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- Citations: 91
Allen DA, Spyromilio J, Meikle WPS, et al., 1988, Supernova 1987A in the Large Magellanic Cloud, IAU Circular, 4623
D. Allen, Anglo-Australian Observatory; and J. Spyromilio, P. Meikle, and G. Varani, Imperial College, London, write: "We find a dramatic increase in prominence of the [Ni I] line at 3.119 microns in SN 1987A. In a spectrum taken at the Anglo-Australian Telescope on July 1, the line had about half the intensity of Brackett-alpha. It has been virtually constant since Feb., although the local continuum has fallen fourfold in that time. The line is quite narrow, with FWHM (measured at resolution 400) of 3000 km/s. The companion line at 3.951 microns may also be present in the wing of Brackett-alpha. We encourage observers with access to longer-wavelength transitions of this and similar species to keep the supernova under close scrutiny."
Graham JR, Evans A, Albinson JS, et al., 1988, IRAS Observations of Collisionally Heated Dust in Large Magellanic Cloud Supernova Remnants, IAU Colloq. 101
Matcher S, Meikle WPS, Morgan BL, et al., 1988, Supernova 1987A in the Large Magellanic Cloud, IAU Circular, 4543
S. Matcher, P. Meikle, B. Morgan, H. Vine, J. Spyromilio, and D. Blackmore, Imperial College, London, telex: "We report further observations of SN 1987A made with the Imperial College speckle interferometer under good conditions (seeing about 1") at the Anglo- Australian Telescope on 1987 Oct. 25.7 (at wavelengths 486, 589, and 656 nm with bandwidths of 10, 10, and 9 nm, respectively) and Nov. 25.6 UT (486 nm). We have made a preliminary search of our data for the presence of a second source, the circular search fields being centered on the SN and having radii of 0".47 and 0".83 on Oct. 25 and Nov. 25, respectively; the fields had resolution-limited, circularly-shaped inner boundaries of radii about 0".03 at 486 nm, rising to about 0".04 at 656 nm. No second source was detected at any wavelength on either date; we estimate that any unresolved second source lying in our search fields must have been at least 4 magnitudes fainter than the SN in the passbands."
MEIKLE WPS, 1988, REVIEW OF SPECKLE OBSERVATIONS OF SUPERNOVA 1987A, PROCEEDINGS ASTRONOMICAL SOCIETY OF AUSTRALIA, Vol: 7, Pages: 473-478, ISSN: 0066-9997
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- Citations: 1
MEIKLE WPS, MATCHER SJ, MORGAN BL, 1987, SPECKLE INTERFEROMETRIC OBSERVATIONS OF SUPERNOVA 1987A AND OF A BRIGHT ASSOCIATED SOURCE, NATURE, Vol: 329, Pages: 608-611, ISSN: 0028-0836
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- Citations: 50
GRAHAM JR, EVANS A, ALBINSON JS, et al., 1987, IRAS OBSERVATIONS OF COLLISIONALLY HEATED DUST IN LARGE MAGELLANIC CLOUD SUPERNOVA-REMNANTS, ASTROPHYSICAL JOURNAL, Vol: 319, Pages: 126-135, ISSN: 0004-637X
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- Citations: 30
Meikle W, Matcher SJ, Morgan BL, 1987, Optical Speckle Interferometry of Supernova 1987A, ESO Workshop on the SN 1987 A
Meikle W, Matcher SJ, Morgan BL, 1987, Optical Speckle Interferometric Observations of Supernova 1987A, Bulletin of the American Astronomical Society, Vol. 19, p.950
Graham JR, Wright GS, Joseph RD, et al., 1987, Star Formation in the Merging Galaxy NGC325, Star formation in galaxies
Meikle WPS, Matcher S, Morgan BL, 1987, Supernova 1987A in the Large Magellanic Cloud, IAU Circular, 4369
P. Meikle, Imperial College, London, telexes: "S. Matcher, B. Morgan, and I carried out speckle interferometric observations of SN 1987A using the Imperial College speckle interferometer at the Anglo-Australian Telescope on Apr. 2.41-2.48 UT. Filter passbands were 1.5 nm, centered on 386.9 and 486.1 (H-beta) nm. Preliminary data reduction indicates that the SN was unresolved at either wavelength, implying angular radii of < about 0".012 and 0".015, respectively. The corresponding limits on the linear radius are 9 x 10E13 and 11 x 10E13 m, respectively (d_LMC = 50 kpc), consistent with the radii implied by spectroscopically derived velocities."
Suntzeff N, Hamuy M, Meikle WPS, et al., 1987, Supernova 1987A in the Large Magellanic Cloud, IAU Circulars, 4369
N. Suntzeff and M. Hamuy, Cerro Tololo Interamerican Observatory, report: "Our nightly photoelectric observations at CTIO in the Cousins UBVRI system show that SN 1987A has begun to brighten in U. Since Mar. 26 (through Apr. 19), the SN has brightened in BVRI by 0.029 mag/day in a remarkably linear fashion. Beginning about Apr. 15, U has brightened by about 0.03 mag/day. From published infrared colors and measurements taken at CTIO, the SN has been increasing in bolometric luminosity by 2.8 percent/day since one week after outburst. On Apr. 19.0 UT, we observed the following colors: V = 3.30, B-V = +1.65, U-B = +2.65, V-R = +0.70, R-I = +0.27." P. Meikle, Imperial College, London, telexes: "S. Matcher, B. Morgan, and I carried out speckle interferometric observations of SN 1987A using the Imperial College speckle interferometer at the Anglo-Australian Telescope on Apr. 2.41-2.48 UT. Filter passbands were 1.5 nm, centered on 386.9 and 486.1 (H-beta) nm. Preliminary data reduction indicates that the SN was unresolved at either wavelength, implying angular radii of < about 0".012 and 0".015, respectively. The corresponding limits on the linear radius are 9 x 10E13 and 11 x 10E13 m, respectively (d_LMC = 50 kpc), consistent with the radii implied by spectroscopically derived velocities." Provisional photometry by A. Beresford, Adelaide, South Australia (20-cm reflector): Apr. 17.4 UT, V = 3.24, B-V = +1.69; 18.44, 3.19, +1.67; 20.46, 3.15, +1.62. Corrigendum: On IAUC 4366, the magnitude estimate by M. Morel should read 3.4.
Meikle W, Graham J, Gregory B, et al., 1987, Supernova 1987A in the Large Magellanic Cloud, IAU Circulars, 4354
We have obtained infrared photometry and spectroscopy of SN 1987A during Mar. 15.04- 15.09 UT using the cooled grating spectrometer (resolution 500) on the CTIO 4-m telescope. The infrared magnitudes were J = 2.64, H = 2.40, K = 2.20, and L = 1.73, corresponding to fluxes that are about 60 percent brighter than those reported on IAUC 4347 for Mar. 5-8. H I lines observed were 5-3, 5-4, 7-4, and 8-5; all these lines exhibit broad P-Cyg profiles. The rest-wavelength to trough- wavelength velocity differences are considerably lower than those derived from lower series (Balmer) lines at the same epoch, and are about 60 percent of the velocities observed in the same infrared lines on Mar. 5-8 (IAUC 4347). The low infrared line velocities suggest that they are formed much closer to the region of continuum emission than are the Balmer lines, and that this region was already deep within the ejecta in mid-Mar." M. G. Pastoriza and T. Scorchi-Bergmann, Instituto de Fisica, Universidad Federal Rio Grande do Sul, report: "Using the CTIO 1-m telescope (+ 2D-Frutti detector), we observed the spectral region 370-700 nm (resolution 0.5 nm) during Feb. 25-Mar. 5, and have obtained flux values (comparison star eta Hya) for four wavelengths selected to represent the continuum: 442 nm was chosen between the emission lines of H-gamma and Fe II (458.3 nm), and the others are from regions free of lines. The standard deviations of the flux values obtained for the comparison star delta Dor during the seven nights are: 442 nm, 4; 535 nm, 4; 585 nm, 4; 702 nm, 16. The fluxes are given in units of 10E-11 ergs/s/cm**2/A: Feb. 27.01 UT, F(442 nm) = 8.4, F(535 nm) = 6.4, F(585 nm) = 5.6, F(702 nm) = 4.4; 28.01, 7.4, 6.4, 5.2, 4.0; Mar. 1.07, 5.9, 5.1, 4.3, 2.5; 2.06, 5.0, 5.7, 5.2, 2.5; 3.04, 5.0, 6.2, 5.6, 3.2; 4.02, 4.8, 6.2, 5.8, 3.0; 5.01, 4.3, 6.9, 6.4, 2.9. The estimated maximum of the flux distribution shifted from 420 nm on Feb. 27 to 520 nm on Mar. 5.
Matcher SJ, Meikle WPS, Morgan BL, et al., 1987, Supernova 1987A in the Large Magellanic Cloud, IAU Circular, 4391
S. J. Matcher, W. P. S. Meikle, and B. L. Morgan, Imperial College, London, telex: "We report further observations (cf. IAUC 4369) of SN 1987A at the Anglo-Australian Telescope on Apr. 14.42- 14.45 UT using the Imperial College speckle interferometer. Filter passbands were 1.0 nm, centered on 587.6 nm and 658 nm. At 658.5 nm, a source was detected at p.a. 196 deg +/- 2 deg. Preliminary examination of the data suggests that the source is about 3 mag fainter than the SN at this wavelength. At 587.6 nm, there is marginal evidence for the presence of a source at the same position but of fainter magnitude. To within the quoted errors, the position of the source is the same as that reported on IAUC 4382. Observations of a nearby reference star (BS 2015), made immediately before and after the SN observations, yielded autocorrelation functions corresponding to an unresolved source." Photoelectric photometry by S. O. Kepler, Instituto de Fisica, Universidad Federal Rio Grande do Sul (0.5-m telescope): May 10.96 UT, V = 3.29, B = 4.78 (+/- 0.05).
GRAHAM JR, MEIKLE WPS, 1986, ANALYSIS OF THE INFRARED ECHO OF SUPERNOVA 1982E IN NGC 1332, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 221, Pages: 789-807, ISSN: 0035-8711
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- Citations: 41
Blanco VM, Aycock J, Baas F, et al., 1986, Supernova 1986G in NGC 5128, IAU Circulars, 4224
V. M. Blanco, Cerro Tololo Interamerican Observatory, reports the following photometric measurements, obtained on May 11.09 UT: V = 11.46, B-V = +1.02, V-B = +0.78, V-I (Cousins) = +0.85. J. Aycock, F. Baas, M. F. Bode, T. R. Geballe, A. J. Longmore, A. D. MacFadzean, M. G. Smith and D. M. Walther, in collaboration with J. R. Graham and W. P. S. Meikle, report: "A 7-channel cooled grating spectrometer, mounted on the U.K. Infrared Telescope, Mauna Kea, was used to measure spectra in the J, H and K windows on May 24, 25 and 26, respectively. The spectra show many prominent, broad, absorption/emission features in each band, to an extent that makes the continuum difficult to define. Of particular note is a very broad and deep 'absorption' that appears to extend from 1.20 to 1.55 microns (FWHM). However, at present our spectra do not cover the region from 1.36 to 1.49 microns, so the intensity could peak again in the unobserved spectral region. The short-wavelength end of this remarkable feature is clearly responsible for the extremely red J-H colors of classical type I supernovae at this epoch. At first sight the explanation of the red J-H colors as due to absorption by Si I 1.203 micron (Graham 1986, M.N.R.A.S. 220, 27P) seems unlikely because the wavelength of the absorption should be blueshifted by ~ 10 000 km/s and consequently should occur at 1.16 microns." Visual magnitude estimates by R. O. Evans (E), Hazelbrook, and R. H. McNaught (M), Coonabarabran, N.S.W., the first six correcting those on IAUC 4208: May 3.5 UT, 12.0 (E); 3.545, 11.8 (M); 3.589, 11.9 (M); 4.5, 12.5 (E); 4.507, 12.4 (M); 4.654, 11.8 (M); 6.6, 11.8 (E); 7.35, 12.3 (E); 8.5, 12.0 (E); 9.5, 12.0 (E); 10.5, 11.9 (E); 11.5, 11.6 (E); 12.4, 11.6 (E); 13.63, 11.8 (M); 14.53, 11.7 (M); 15.38, 11.6 (M); 16.39, 11.8 (M); 18.61, 11.8 (M); 20.65, 11.9 (M); 21.49, 12.2 (M); 28.48, 12.7 (M); 29.46, 12.9 (M); 30.47, 12.8 (M); 31.41, 13.3 (M); June 1.51, 13.5 (M).
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