Publications
182 results found
Kotak R, Meikle P, van Dyk SD, et al., 2005, Early-time <i>Spitzer</i> observations of the type II plateau supernova SN 2004dj, ASTROPHYSICAL JOURNAL, Vol: 628, Pages: L123-L126, ISSN: 0004-637X
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- Citations: 49
Kotak R, Meikle WPS, Pignata G, et al., 2005, Spectroscopy of the type Ia supernova SN 2002er: Days-11 to+215, ASTRONOMY & ASTROPHYSICS, Vol: 436, Pages: 1021-1031, ISSN: 1432-0746
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- Citations: 52
Meikle W, 2005, The Observations of Dust in Supernova Explosions, Bulletin of the American Astronomical Society, Vol. 37, p.470, Publisher: American Astronomical Society Meeting 206
For over thirty years it has been hypothesised that core-collapse supernovae are, or have been, a major source of dust in the universe. However, only in a very few cases has dust condensation in supernova ejecta been directly and convincingly demonstrated. Two methods are employed. In one procedure, the relative fading of the red wings of the broad optical or near-infrared spectral lines is used to infer the formation of attenuating dust. In the other method, evidence of newly-formed grains can be sought via thermal infrared emission. The characteristic temperature of condensing dust peaks in the mid-infrared region. However, apart from the exceptionally nearby SN 1987A, we have only recently been able to seek mid-infrared emission from supernovae. This has been made feasible by the advent of new infrared facilities, especially the Spitzer Space Telescope. To use the infrared flux from a supernova to demonstrate grain condensation, we must proceed cautiously. At least 10 core-collapse supernovae have shown late-time near-infrared emission implying the presence of hot dust. But in many cases the radiation may have been due to an infrared "echo" i.e. if the progenitor produces a dusty wind, the early-time luminosity of the supernova can heat this dust yielding a high infrared luminosity. To distinguish between the condensation and IR-echo scenarios it is important to monitor the infrared emission over a wide spectral and temporal range. Ground-based monitoring of the Type IIn SN 1998S out to a wavelength of 4.7 microns has provided some of the most convincing evidence to date about the occurrence and location of dust formation in supernova ejecta. While the near-infrared range is valuable, potentially the most useful information lies in the largely unexplored region at even longer wavelengths. The Spitzer Space Telescope has started to provide this vital information.
Hendry MA, Smartt SJ, Maund JR, et al., 2005, A study of the Type II-P supernova 2003gd in M74, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 359, Pages: 906-926, ISSN: 0035-8711
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- Citations: 100
Mattila S, Greimel R, Meikle W, 2005, LIRIS Discovers Supernovae in Starburst Galaxies, The Newsletter of the Isaac Newton Group of Telescopes, Pages: 16-17
In the nuclear regions of M82 and other nearby starburst galaxies one core-collapse supernova (CCSN) is expected to explode every 5-10 years. Furthermore, in luminous infrared galaxies (LIRGs) such as the interacting system Arp299 (NGC3690 +IC0694) at least one CCSN can be expected every year. However, due to the high dust extinction astronomers have been unable to detect these SNe. By observing in the near-IR Ks-band the extinction is strongly reduced, making searches for such dust obscured SNe look feasible. In fact, recent near-IR searches have been able to detect a couple of SNe in starburst galaxies. These are however only extinguished by a few of magnitudes in the visual wavelengths. Now also the newly commissioned near-IR imager LIRIS on WHT has discovered two new SNe within the nuclear regions of Arp299 and NGC2146.
Mattila S, Greimel R, Gerardy C, et al., 2005, Supernova 2005V in NGC 2146, IAU Circular, 8474
Further to IAUC 8473, S. Mattila et al. report the discovery of another apparent supernova (mag 13.8) in K_s-band images obtained on Jan. 30.16 UT at the William Herschel Telescope. The new object is located at R.A. = 6h18m38s.28, Decl. = +78o21'28".8 (equinox 2000.0), which is 1".8 east and 3".4 north of the K_s-band nucleus of the starburst galaxy NGC 2146. J- and H-band observations of SN 2005V yield preliminary colors J-H = +0.13 +/- 0.33 and H-K = +0.18 +/- 0.34, indicating modest extinction.
Mattila S, Greimel R, Gerardy C, et al., 2005, Arp 299, IAU Circ., 8477
Further to IAUC 8473, S. Mattila, R. Greimel, C. Gerardy, and W. P. S. Meikle, together with D. L. Clements and K. Nandra (Imperial College, London), report the discovery on a K_s-band image obtained on Jan. 30.3 UT of a strong outburst in the B1 nucleus (Wynn-Williams et al. 1991, Ap.J. 377, 426) of the galaxy Arp 299. The nucleus was not in outburst in their previous such image taken on 2004 June 6.0, and the difference in brightness yields a magnitude for the new source of K_s = +12.6 +/- 0.1; at a distance of 45 Mpc, this translates to M(K_s) about -20.7, which is about a magnitude brighter than would be expected for the brightest supernovae (cf. Mattila and Meikle 2001, MNRAS 324, 325). The new source is located at R.A. = 11h28m31s.02, Decl. = +58o33'40".7 (equinox 2000.0), which is < 0".1 from the K_s-band nucleus B1 and < 0".5 from the location of the x-ray-determined active galactic nucleus (AGN) in Arp 299 (Ballo et al. 2004, Ap.J. 600, 634). The source is therefore most likely associated with an AGN outburst in the nucleus B1.
Mattila S, Greimel R, Gerardy C, et al., 2005, Supernovae 2005Q, 2005R, 2005S, 2005T, 2005U, IAU Circular, 8473
Several apparent new supernovae have been reported, all on unfiltered CCD images except for 2005U, which was found by S. Mattila (Stockholm Observatory), R. Greimel (Isaac Newton Group of Telescopes), and C. Gerardy and W. P. S. Meikle (Imperial College, London) on K_s-band images obtained as part of the ongoing 'Nuclear Supernova Search' campaign with the William Herschel Telescope (+ LIRIS). SN 2005Q was found by L. A. G. Monard (cf. IAUC 8454), and SN 2005R was found by T. Boles (cf. IAUC 8469), while 2005S and 2005T were found by H. Pugh, J. Graham, and W. Li (LOSS/KAIT; cf. IAUC 8472). SN 2005 UT R.A. (2000.0) Decl. Mag. Offset 2005Q Jan. 28.803 1 30 03.51 -42 40 48.4 17.2 22" W, 20" N 2005R Jan. 13.971 11 14 56.81 +33 49 35.7 17.4 0".9 W, 3".2 N 2005S Jan. 22.58 14 08 28.84 + 7 03 27.2 19.1 5".6 W, 0".9 S 2005T Jan. 24.54 14 26 17.24 +26 14 47.8 18.4 7".2 W, 0".9 N 2005U Jan. 30.30 11 28 33.22 +58 33 42.5 16.2 3".7 W, 4".9 S Additional approximate unfiltered CCD magnitudes, by the respective discoverers unless noted otherwise: SN 2005Q in ESO 244-G31, 2004 Dec. 30.814 UT, [18.7; Jan. 29.757, 17.1 +/- 0.2. SN 2005R in UGC 6274, 2004 Apr. 22, [19.5; Nov. 13, [19.5; 2005 Jan. 16.052, 17.4. SN 2005S in UGC 9037, 2004 June 24.21, [20.0; 2005 Jan. 24.59, 19.2. SN 2005T in IC 4423, 2004 June 27.21, [19.5; 2005 Jan. 31.53, 18.3. SN 2005U in Arp 299, 2004 Dec. 25.41, [18.8 (Li, KAIT); Jan. 23.40, 18.2 (Li, KAIT).
Kotak R, Meikle WPS, 2005, Optical and near-infrared observations of SN 2002ic, Conference on 1604-2004 - Supernovae as Cosmological Lighthouses, 15 - 19 June 2004, Padua, ITALY, Publisher: Astronomical Soc Pacific, Pages: 264-265
Meikle P, Khreegi Y, Kotak R, 2005, Multiband observations of type Ia supernovae at late times, Conference on 1604-2004 - Supernovae as Cosmological Lighthouses, 15 - 19 June 2004, Padua, ITALY, Publisher: Astronomical Soc Pacific, Pages: 217-223
Pozzo M, Meikle WPS, Fassia A, et al., 2005, Dust signatures from late-time infrared and optical observations of SN1998S, Conference on 1604-2004 - Supernovae as Cosmological Lighthouses, 15 - 19 June 2004, Univ Degli Studi Padova, Padua, ITALY, Publisher: Astronomical Soc Pacific, Pages: 337-340
Pignata G, Patat F, Benetti S, et al., 2004, Photometric observations of the Type Ia SN 2002er in UGC 10743, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 355, Pages: 178-190, ISSN: 0035-8711
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- Citations: 63
Kotak R, Meikle WPS, Adamson A, et al., 2004, On the nature of the circumstellar medium of the remarkable Type Ia/IIn supernova SN 2002ic, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 354, Pages: L13-L17, ISSN: 0035-8711
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- Citations: 62
Pozzo M, Meikle WPS, Fassia A, et al., 2004, On the source of the late-time infrared luminosity of SN1998S and other Type II supernovae, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 352, Pages: 457-477, ISSN: 0035-8711
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- Citations: 123
Pignata G, Patat F, Kotak R, et al., 2004, ESC Observations of SN 2002er around Maximum Light, Supernovae (10 years of 1993J)
Mattila S, Meikle WPS, Greimel R, 2004, Highly extinguished supernovae in the nuclear regions of starburst galaxies, Workshop on Supernovae and Dust, Publisher: ELSEVIER SCI LTD, Pages: 595-600, ISSN: 1387-6473
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- Citations: 22
Stathakis R, Mattila S, Cannon R, et al., 2004, Optical studies of the ring around SN 1987A, Anglo-Australian Observatory Newsletter, No. 104
Mattila S, Meikle W, Groeningsson P, et al., 2004, Supernova 2004am in M82, IAU Circular, 8299
S. Mattila, Stockholm Observatory; W. P. S. Meikle, Imperial College, London; P. Groeningsson, Stockholm Observatory; R. Greimel and M. Schirmer, Isaac Newton Group of Telescopes; and J. A. Acosta-Pulido, Instituto de Astrofisica de Canarias, obtained infrared images and spectra of SN 2004am (IAUC 8297) on Mar. 6.9 UT, using LIRIS on the William Herschel Telescope (WHT). Preliminary reduction of the 0.89-1.53-micron spectrum shows discrete features superimposed on a significant continuum sloping slightly upwards to longer wavelengths. Emission lines of Paschen_gamma and Paschen_beta are seen, having FWZI of about 2800 km/s. It is concluded that this is a type-II supernova, but probably highly reddened within the starburst galaxy M82. The spectrum has some similarity to that of the type-IIP supernova 1995V (Fassia et al. 1998, MNRAS 299, 150) at about 85 days. A preliminary magnitude of K_s = 12 was estimated for the supernova via image-subtraction techniques, using a reference K_s-band image obtained on 2002 Jan. 3.0 with the WHT (+ INGRID) as part of the ongoing 'Nuclear Supernova Search' campaign. Adopting the unfiltered magnitude (m_u) from IAUC 8297 yields a color of m_u-K about +5. This indicates a high extinction for the supernova, as already suggested by W. Li (private comm.), corresponding to a visual extinction of about 5 magnitudes.
Benetti S, Meikle P, Stehle M, et al., 2004, Supernova 2002bo: inadequacy of the single parameter description, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 348, Pages: 261-278, ISSN: 0035-8711
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- Citations: 176
Meikle W, Mattila S, Carter D, et al., 2004, Supernova 2004C in NGC 3683, IAU Circular, 8270
W. P. S. Meikle, Imperial College, London; and S. Mattila, Stockholm Observatory, report observations of SN 2004C carried out by D. Carter and R. J. Smith, Liverpool John Moores University, on Jan. 16.2 UT using the Liverpool Telescope (+ RATCam) on La Palma. Preliminary photometry yields the following values: g' = 18.31, r' = 16.74, i' = 16.37, z' = 16.12 (uncertainties about +/- 0.05 mag). Comparison of the g'-r' and r'-i' colors with the intrinsic g-r and r-i values for a type-Ic supernova (Poznanski et al. 2002, PASP 114, 833, Fig. 8) at 3 weeks past maximum light (cf. IAUC 8269) indicates an extinction exceeding A_v = 1.0.
Pastorello A, Zampieri L, Turatto M, et al., 2004, Low-luminosity Type II supernovae: spectroscopic and photometric evolution, MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Vol: 347, Pages: 74-94, ISSN: 0035-8711
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- Citations: 198
Mattila S, Lundqvist P, Meikle W, et al., 2003, The Iron Abundance and Density Structure of the Inner Ring around SN 1987A, Supernovae (10 Years of SN1993J)
Kotak R, Meikle W, Smartt S, et al., 2003, Supernova 2003gd in M74, IAU Circular, 8152
R. Kotak and W. P. S. Meikle, Imperial College, London, and S. J. Smartt, Institute of Astronomy, Cambridge, on behalf of the European Supernova Collaboration, report that a spectrum (range about 400-840 nm) of SN 2003gd was obtained at the William Herschel Telescope (+ ISIS spectrograph) by C. Benn on June 14.2 UT. Comparison of a preliminary reduction of the spectrum with spectra of SN 1992H and SN 1987A (Filippenko 1997, ARAA 35, 309) indicates that the new supernova is of type II, roughly 2 months post- explosion. The strong H_alpha P-Cyg profile extends from -8800 to +7100 km/s in the host-galaxy rest frame.
Kotak R, Meikle W, Rodriguez-Gil P, et al., 2003, Supernova 2003dv in UGC 9638, IAU Circular, 8124
R. Kotak and W. P. S. Meikle, Imperial College, London, on behalf of the European Supernova Collaboration, report that spectra (resolution 0.27 nm) of the possible supernova reported on IAUC 8121, obtained at the Isaac Newton Telescope (+ IDS spectrograph) by P. Rodriguez-Gil on Apr. 26.11 (range about 500-750 nm) and Apr. 27.06 UT (range about 350-570 nm), indicate that it is of type IIn, about 1 week past explosion. The spectrum comprises a blue continuum upon which a number of emission features are superposed. The continuum appears to show a break at about 530 nm, blueward of which it becomes steeper. The spectrum lacks broad P-Cyg-type profiles and bears a striking resemblance to early-epoch spectra of the type-IIn SN 1998S (IAUC 6829; Leonard et al. 1999, Ap.J. 536, 239; Fassia et al. 2001, MNRAS 325, 907). Balmer lines in emission are present and exhibit a multicomponent structure. The H_alpha profile comprises a narrow but resolved component (FWHM about 350 km/s) superposed on a much broader profile of FWZI about 10000 km/s. The narrow component appears to lie slightly redward (about 350 km/s) of the peak of the broad component. A broad emission feature at about 470 nm is present, which is attributed to a blend of He II 468.6-nm and C III 464.8-nm/N III 464.0-nm (cf. SN 1998S; IAUC 6832). A weak He I 587.6-nm emission feature may also be present. In SN 1998S, the early-time emission features yielded valuable information about the interaction of the supernova with the 'circumstellar medium' of the progenitor star, but these features persisted for barely 10 days. High-resolution spectral coverage over the next few days is urged.
Kotak R, Meikle W, Rodriguez-Gil P, et al., 2003, Supernova 2003du in UGC 9391, IAU Circular, 8122
R. Kotak and W. P. S. Meikle, Imperial College, London, on behalf of the European Supernova Collaboration, report that a spectrum (range about 500-760 nm) of SN 2003du (cf. IAUC 8121), obtained at the Isaac Newton Telescope (+ IDS spectrograph) by P. Rodriguez-Gil on Apr. 24.06 UT, shows the characteristic Si II 615- nm absorption feature indicating that it is of type Ia. Comparison with the spectra of SN 2002bo indicates a phase of approximately 2 weeks before maximum light (-13 +/- 2 days). The depths of the features, relative to the continuum, appear somewhat more shallow than in SN 2002bo.
Kotak R, Meikle W, Patat F, et al., 2003, Supernova 2003cg in NGC 3169, IAU Circular, 8099
R. Kotak and W. P. S. Meikle, Imperial College, London; and F. Patat, European Southern Observatory, on behalf of the European Supernova Collaboration, report that a spectrum (range 427-686 nm) of SN 2003cg (cf. IAUC 8097), obtained at the William Herschel Telescope (+ ISIS) by G. Nelemans on Mar. 22.9 UT, shows it to be a highly-reddened 'normal' type-Ia supernova, a few days before maximum (compared to SN 1994D; Patat et al. 1996, MNRAS 278, 111), with a total extinction of A_v about 2.5 magnitudes. Very strong, multicomponent Na I D interstellar absorption lines are present in the rest frame of the host galaxy.
Pastorella A, Baron E, Benetti S, et al., 2003, Faint Core-Collapse Supernovae, From Twilight to Highlight: The Physics of Supernovae
Meikle P, Fassia A, Geballe TR, et al., 2003, The dusty type IIn supernova 1998S, Berlin, Workshop on from twilight to highlights - the physics of supernovae, Garching, Germany, 29 - 31 July 2002, Publisher: Springer-Verlag, Pages: 229-236
Mattila S, Meikle P, Greimel R, 2003, The search for nuclear supernovae, Workshop on From Twilight to Highlights - The Physics of Supernovae, Publisher: SPRINGER-VERLAG BERLIN, Pages: 391-394
Meikle W, Mattila S, Smartt S, et al., 2002, Supernova 2002hh in NGC 6946, IAU Circular, 8024
P. Meikle, Imperial College, London; S. Mattila, Stockholm Observatory; and S. Smartt, Institute of Astronomy, Cambridge, report that infrared observations of the type-II supernova 2002hh obtained by E. MacDonald, L. Clewley, and G. Dalton at the William Herschel Telescope (+ infrared camera INGRID) on Nov. 18.86 UT yield J = 12.30 +/- 0.03, K_s = 11.07 +/- 0.02. Adopting a phase of 21 +/- 2 days post-explosion, comparison of the J-K_s color with the infrared-template light curves of Mattila and Meikle (2001, MNRAS 324, 325) indicates that the supernova is highly reddened, with E(J-K_s) = 1.0, confirming the result of Filippenko et al. (IAUC 8007). Using the reddening law of Cardelli et al. (1989, Ap.J. 345, 245), this yields A(V) about 6.1. Subtracting the Galactic extinction (Schlegel et al. 1998, Ap.J. 500, 525) yields a host-galaxy extinction A(V) about 5.0. Adopting a distance of 5.9 Mpc (H_0 = 70; Tully 1988, Nearby Galaxies Catalog) yields de- reddened absolute magnitudes of M(J) = -18.3 and M(K_s) = -18.5, which are close to the values given by the templates of Mattila and Meikle (2001).
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