-
4
-
-
0001071170
-
-
R. Sunyaev et al., Nature 330, 227 (1987).
-
(1987)
Nature
, vol.330
, pp. 227
-
-
Sunyaev, R.1
-
5
-
-
0000210109
-
-
T. Dotani et al., Nature 330, 230 (1987).
-
(1987)
Nature
, vol.330
, pp. 230
-
-
Dotani, T.1
-
8
-
-
0000517052
-
-
W. D. Arnett, J. N. Bahcall, R. P. Kirshner, S. E. Woosley, Annu. Rev. Astron. Astrophys. 27, 629 (1989).
-
(1989)
Annu. Rev. Astron. Astrophys.
, vol.27
, pp. 629
-
-
Arnett, W.D.1
Bahcall, J.N.2
Kirshner, R.P.3
Woosley, S.E.4
-
13
-
-
0005814307
-
-
S. H. Moseley et al., Nature 340, 697 (1989).
-
(1989)
Nature
, vol.340
, pp. 697
-
-
Moseley, S.H.1
-
16
-
-
0039436332
-
-
Structure and Dynamics of the Interstellar Medium, Proceedings of IAU Colloq. 120, G. Tenorio-Tagle, M. Moles, J. Melnick, Eds., Also
-
L. B. Lucy, I. J. Danziger, C. Gouiffes, P. Bouchet, in Structure and Dynamics of the Interstellar Medium, Proceedings of IAU Colloq. 120, G. Tenorio-Tagle, M. Moles, J. Melnick, Eds., Also Lecture Notes in Physics, vol 350 (1989), pp. 164-179.
-
(1989)
Lecture Notes in Physics
, vol.350
, pp. 164-179
-
-
Lucy, L.B.1
Danziger, I.J.2
Gouiffes, C.3
Bouchet, P.4
-
25
-
-
80052464947
-
-
note
-
We combined the two observations because there were no substantial changes in the fluxes seen in the two epochs. The basic steps for the data processing of the PACS and SPIRE data are described by (24). Despite the subtraction of the baseline, residual striping remained along the scan direction of the PACS maps. To mitigate the stripes, we subtracted from the PACS images an image of the striping, produced by unambiguously identifying the power spectrum associated with the stripes in Fourier space. The HERITAGE astrometric reference frame is tied to the Two Micron All Sky Survey (2MASS) (44), which has an accuracy of 0.3″ (1 SD), through the Spitzer mid-infrared LMC data (45).
-
-
-
-
27
-
-
80052485762
-
-
note
-
We used the Starfinder software (46), which employs PSF fitting on complex backgrounds. The SPIRE PSFs are empirical models derived from scan-map data for Neptune (47). For PACS, we used empirical model PSFs, based on maps of Vesta (48).
-
-
-
-
28
-
-
77952900012
-
-
R. Sturm, F. Haberl, B. Aschenbach, G. Hasinger, Astron. Astrophys. 515, A5 (2010).
-
(2010)
Astron. Astrophys.
, vol.515
-
-
Sturm, R.1
Haberl, F.2
Aschenbach, B.3
Hasinger, G.4
-
30
-
-
80052433317
-
-
note
-
-1) using Mie theory. In the far-infrared/submm wavelength regime, κ is independent of grain radius up to ∼5 μm, except for metallic iron, for which the absorption efficiency depends on the relative sizes of the skin depth and grain radius. The entries for metallic iron were calculated for a nominal radius of 0.1 μm and a radius of 0.5 μm, for which the value of κ is a maximum in the Herschel wavelength range. The iron mass for this radius thus represents a minimum required mass to fit the observations.
-
-
-
-
31
-
-
80052455984
-
-
note
-
We assumed that the silicon, iron, and magnesium elemental abundances before the explosion were the same as those of the ISM and that these abundances limited the dust mass. We adopted an ISM gas-to-dust mass ratio of 300 because it is higher in the LMC than in the Milky Way (55), where it is typically 100.
-
-
-
-
33
-
-
80052455022
-
-
note
-
These dust temperatures have some dependence on the grain size and the grain compositions.
-
-
-
-
36
-
-
79959559504
-
-
J. Larsson et al., Nature 474, 484 (2011).
-
(2011)
Nature
, vol.474
, pp. 484
-
-
Larsson, J.1
-
45
-
-
33845945133
-
-
M. Meixner et al., Astron. J. 132, 2268 (2006).
-
(2006)
Astron. J.
, vol.132
, pp. 2268
-
-
Meixner, M.1
-
48
-
-
80052430001
-
-
PACS Observer's Manual; http://herschel.esac.esa.int/Docs/PACS/html/pacs- om.html.
-
PACS Observer's Manual
-
-
-
50
-
-
1542396787
-
-
V. G. Zubko, V. Mennella, L. Colangeli, E. Bussoletti, Mon. Not. R. Astron. Soc. 282, 1321 (1996).
-
(1996)
Mon. Not. R. Astron. Soc.
, vol.282
, pp. 1321
-
-
Zubko, V.G.1
Mennella, V.2
Colangeli, L.3
Bussoletti, E.4
-
51
-
-
0242354967
-
-
D. Semenov, T. Henning, C. Helling, M. Ilgner, E. Sedlmayr, Astron. Astrophys. 410, 611 (2003).
-
(2003)
Astron. Astrophys.
, vol.410
, pp. 611
-
-
Semenov, D.1
Henning, T.2
Helling, C.3
Ilgner, M.4
Sedlmayr, E.5
-
55
-
-
0141792454
-
-
K. D. Gordon, G. C. Clayton, K. A. Misselt, A. U. Landolt, M. J. Wolff, Astrophys. J. 594, 279 (2003).
-
(2003)
Astrophys. J.
, vol.594
, pp. 279
-
-
Gordon, K.D.1
Clayton, G.C.2
Misselt, K.A.3
Landolt, A.U.4
Wolff, M.J.5
-
56
-
-
0034632280
-
-
N. Panagia, M. Romaniello, S. Scuderi, R. P. Kirshner, Astrophys. J. 539, 197 (2000).
-
(2000)
Astrophys. J.
, vol.539
, pp. 197
-
-
Panagia, N.1
Romaniello, M.2
Scuderi, S.3
Kirshner, R.P.4
-
57
-
-
77957374252
-
-
K. France et al., Science 329, 1624 (2010).
-
(2010)
Science
, vol.329
, pp. 1624
-
-
France, K.1
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